[{"day":"01","oa_version":"Preprint","external_id":{"arxiv":["1811.00556"]},"month":"10","extern":"1","date_published":"2019-10-01T00:00:00Z","volume":489,"oa":1,"year":"2019","arxiv":1,"abstract":[{"lang":"eng","text":"We investigate the clustering and halo properties of ∼5000 Ly α-selected emission-line galaxies (LAEs) from the Slicing COSMOS 4K (SC4K) and from archival NB497 imaging of SA22 split in 15 discrete redshift slices between z ∼ 2.5 and 6. We measure clustering lengths of r0 ∼ 3–6 h−1 Mpc and typical halo masses of ∼1011 M⊙ for our narrowband-selected LAEs with typical LLy α ∼ 1042–43 erg s−1. The intermediate-band-selected LAEs are observed to have r0 ∼ 3.5–15 h−1 Mpc with typical halo masses of ∼1011–12 M⊙ and typical LLy α ∼ 1043–43.6 erg s−1. We find a strong, redshift-independent correlation between halo mass and Ly α luminosity normalized by the characteristic Ly α luminosity, L⋆(z). The faintest LAEs (L ∼ 0.1 L⋆(z)) typically identified by deep narrowband surveys are found in 1010 M⊙ haloes and the brightest LAEs (L ∼ 7 L⋆(z)) are found in ∼5 × 1012 M⊙ haloes. A dependency on the rest-frame 1500 Å UV luminosity, MUV, is also observed where the halo masses increase from 1011 to 1013 M⊙ for MUV ∼ −19 to −23.5 mag. Halo mass is also observed to increase from 109.8 to 1012 M⊙ for dust-corrected UV star formation rates from ∼0.6 to 10 M⊙ yr−1 and continues to increase up to 1013 M⊙ in halo mass, where the majority of those sources are active galactic nuclei. All the trends we observe are found to be redshift independent. Our results reveal that LAEs are the likely progenitors of a wide range of galaxies depending on their luminosity, from dwarf-like, to Milky Way-type, to bright cluster galaxies. LAEs therefore provide unique insight into the early formation and evolution of the galaxies we observe in the local Universe."}],"article_type":"original","publication_status":"published","main_file_link":[{"url":"https://arxiv.org/abs/1811.00556","open_access":"1"}],"publisher":"Oxford University Press","_id":"11535","doi":"10.1093/mnras/stz2149","author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"full_name":"Sobral, D","first_name":"D","last_name":"Sobral"},{"first_name":"B","last_name":"Mobasher","full_name":"Mobasher, B"},{"last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Cochrane, R K","last_name":"Cochrane","first_name":"R K"},{"full_name":"Chartab, N","first_name":"N","last_name":"Chartab"},{"full_name":"Jafariyazani, M","first_name":"M","last_name":"Jafariyazani"},{"first_name":"A","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, A"},{"first_name":"S","last_name":"Santos","full_name":"Santos, S"},{"full_name":"Calhau, J","last_name":"Calhau","first_name":"J"}],"date_created":"2022-07-07T13:01:03Z","type":"journal_article","intvolume":" 489","issue":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"scopus_import":"1","citation":{"ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 2019;489(1):555-573. doi:10.1093/mnras/stz2149","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Matthee, J. J., Cochrane, R. K., Chartab, N., … Calhau, J. (2019). The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2149","ieee":"A. A. Khostovan et al., “The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities,” Monthly Notices of the Royal Astronomical Society, vol. 489, no. 1. Oxford University Press, pp. 555–573, 2019.","short":"A.A. Khostovan, D. Sobral, B. Mobasher, J.J. Matthee, R.K. Cochrane, N. Chartab, M. Jafariyazani, A. Paulino-Afonso, S. Santos, J. Calhau, Monthly Notices of the Royal Astronomical Society 489 (2019) 555–573.","chicago":"Khostovan, A A, D Sobral, B Mobasher, Jorryt J Matthee, R K Cochrane, N Chartab, M Jafariyazani, A Paulino-Afonso, S Santos, and J Calhau. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz2149.","mla":"Khostovan, A. A., et al. “The Clustering of Typical Ly α Emitters from z ∼ 2.5–6: Host Halo Masses Depend on Ly α and UV Luminosities.” Monthly Notices of the Royal Astronomical Society, vol. 489, no. 1, Oxford University Press, 2019, pp. 555–73, doi:10.1093/mnras/stz2149.","ista":"Khostovan AA, Sobral D, Mobasher B, Matthee JJ, Cochrane RK, Chartab N, Jafariyazani M, Paulino-Afonso A, Santos S, Calhau J. 2019. The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities. Monthly Notices of the Royal Astronomical Society. 489(1), 555–573."},"page":"555-573","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"date_updated":"2022-08-19T06:38:42Z","acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that helped improve this study. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. JM acknowledges support from the ETH Zwicky fellowship. RKC acknowledges funding from STFC via a studentship. APA acknowledges support from the Fundac¸ao para a Ci ˜ encia e a Tecnologia FCT through the fellowship PD/BD/52706/2014 and the research grant UID/FIS/04434/2013. JC and SS both acknowledge their support from the Lancaster University PhD Fellowship. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, SCIPY, MATPLOTLIB, SCIKIT-LEARN, and ASTROPY packages, as well as the TOPCAT analysis program. The SC4K samples used in this paper are all publicly available for use by the community (Sobral et al. 2018a). The catalogue is also available on the COSMOS IPAC website (https://irsa.ipac.caltech.edu/data/COSMOS/overview.html).","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"title":"The clustering of typical Ly α emitters from z ∼ 2.5–6: Host halo masses depend on Ly α and UV luminosities","article_processing_charge":"No"},{"article_processing_charge":"No","title":"The origin of scatter in the star formation rate–stellar mass relation","acknowledgement":"JM acknowledges the support of a Huygens PhD fellowship from Leiden University. We thank Camila Correa for help analysing snipshot merger trees. We thank the anonymous referee for constructive comments. We also thank Jarle Brinchmann, Rob Crain, Antonios Katsianis, Paola Popesso, and David Sobral for discussions and suggestions. We also thank the participants of the Lorentz Center workshop ‘A Decade of the Star-Forming Main Sequence’ held on 2017 September 4–8, for discussions and ideas. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, and SCIPY (Hunter 2007) packages and the TOPCAT analysis tool (Taylor 2013).","date_updated":"2024-10-14T11:33:52Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","citation":{"apa":"Matthee, J. J., & Schaye, J. (2019). The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz030","ama":"Matthee JJ, Schaye J. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 2019;484(1):915-932. doi:10.1093/mnras/stz030","ieee":"J. J. Matthee and J. Schaye, “The origin of scatter in the star formation rate–stellar mass relation,” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1. Oxford University Press, pp. 915–932, 2019.","short":"J.J. Matthee, J. Schaye, Monthly Notices of the Royal Astronomical Society 484 (2019) 915–932.","chicago":"Matthee, Jorryt J, and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz030.","mla":"Matthee, Jorryt J., and Joop Schaye. “The Origin of Scatter in the Star Formation Rate–Stellar Mass Relation.” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 1, Oxford University Press, 2019, pp. 915–32, doi:10.1093/mnras/stz030.","ista":"Matthee JJ, Schaye J. 2019. The origin of scatter in the star formation rate–stellar mass relation. Monthly Notices of the Royal Astronomical Society. 484(1), 915–932."},"page":"915-932","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics : galaxies: evolution","galaxies: formation","galaxies: star formation","cosmology: theory"],"issue":"1","type":"journal_article","intvolume":" 484","author":[{"last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"first_name":"Joop","last_name":"Schaye","full_name":"Schaye, Joop"}],"date_created":"2022-07-08T07:48:31Z","doi":"10.1093/mnras/stz030","_id":"11540","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1805.05956"}],"abstract":[{"lang":"eng","text":"Observations have revealed that the star formation rate (SFR) and stellar mass (Mstar) of star-forming galaxies follow a tight relation known as the galaxy main sequence. However, what physical information is encoded in this relation is under debate. Here, we use the EAGLE cosmological hydrodynamical simulation to study the mass dependence, evolution, and origin of scatter in the SFR–Mstar relation. At z = 0, we find that the scatter decreases slightly with stellar mass from 0.35 dex at Mstar ≈ 109 M⊙ to 0.30 dex at Mstar ≳ 1010.5 M⊙. The scatter decreases from z = 0 to z = 5 by 0.05 dex at Mstar ≳ 1010 M⊙ and by 0.15 dex for lower masses. We show that the scatter at z = 0.1 originates from a combination of fluctuations on short time-scales (ranging from 0.2–2 Gyr) that are presumably associated with self-regulation from cooling, star formation, and outflows, but is dominated by long time-scale (∼10 Gyr) variations related to differences in halo formation times. Shorter time-scale fluctuations are relatively more important for lower mass galaxies. At high masses, differences in black hole formation efficiency cause additional scatter, but also diminish the scatter caused by different halo formation times. While individual galaxies cross the main sequence multiple times during their evolution, they fluctuate around tracks associated with their halo properties, i.e. galaxies above/below the main sequence at z = 0.1 tend to have been above/below the main sequence for ≫1 Gyr."}],"publication_status":"published","article_type":"original","arxiv":1,"volume":484,"date_published":"2019-03-01T00:00:00Z","oa":1,"year":"2019","month":"03","extern":"1","oa_version":"Preprint","external_id":{"arxiv":["1805.05956"]},"day":"01"},{"scopus_import":"1","page":"2422-2441","citation":{"chicago":"Sobral, David, Jorryt J Matthee, Gabriel Brammer, Andrea Ferrara, Lara Alegre, Huub Röttgering, Daniel Schaerer, Bahram Mobasher, and Behnam Darvish. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty2779.","ista":"Sobral D, Matthee JJ, Brammer G, Ferrara A, Alegre L, Röttgering H, Schaerer D, Mobasher B, Darvish B. 2019. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 482(2), 2422–2441.","mla":"Sobral, David, et al. “On the Nature and Physical Conditions of the Luminous Ly α Emitter CR7 and Its Rest-Frame UV Components.” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2, Oxford University Press, 2019, pp. 2422–41, doi:10.1093/mnras/sty2779.","short":"D. Sobral, J.J. Matthee, G. Brammer, A. Ferrara, L. Alegre, H. Röttgering, D. Schaerer, B. Mobasher, B. Darvish, Monthly Notices of the Royal Astronomical Society 482 (2019) 2422–2441.","apa":"Sobral, D., Matthee, J. J., Brammer, G., Ferrara, A., Alegre, L., Röttgering, H., … Darvish, B. (2019). On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2779","ama":"Sobral D, Matthee JJ, Brammer G, et al. On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components. Monthly Notices of the Royal Astronomical Society. 2019;482(2):2422-2441. doi:10.1093/mnras/sty2779","ieee":"D. Sobral et al., “On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components,” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 2. Oxford University Press, pp. 2422–2441, 2019."},"publication":"Monthly Notices of the Royal Astronomical Society","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","cosmology: observations","dark ages","reionization","first stars","early Universe"],"issue":"2","article_processing_charge":"No","acknowledgement":"We thank the anonymous reviewer for the numerous detailed comments that led us to greatly improve the quality, extent, and statistical robustness of this work. DS acknowledges financial support from the Netherlands Organisation for Scientific research through a Veni fellowship. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program, grant number NNX12AE20G and the National Science Foundation, grant number 1716907. We are thankful for several discussions and constructive comments from Johannes Zabl, Eros Vanzella, Bo Milvang-Jensen, Henry McCracken, Max Gronke, Mark Dijkstra, Richard Ellis, and Nicolas Laporte. We also thank Umar Burhanudin and Izzy Garland for taking part in the XGAL internship in Lancaster and for exploring the HST grism data independently. Based on observations obtained with HST/WFC3 programs 12578, 14495, and 14596. Based on observations of the National Japanese Observatory with the Suprime-Cam on the Subaru telescope (S14A-086) on the big island of Hawaii. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France–Hawaii Telescope Legacy Survey, a collaborative project of NRC and CNRS. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A 0786, 093.A-0561, 097.A0043, 097.A-0943, 098.A-0819, 298.A-5012, and 179.A-2005, and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. The authors acknowledge the award of service time (SW2014b20) on the William Herschel Telescope (WHT). WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This research was supported by the Munich Institute for Astro- and Particle Physics of the DFG cluster of excellence ‘Origin and Structure of the Universe’. We have benefitted immensely from the public available programming language PYTHON, including NUMPY and SCIPY (Jones et al. 2001; Van Der Walt, Colbert & Varoquaux 2011), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France. All data used for this paper are publicly available, and we make all reduced data available with the refereed paper.","date_updated":"2022-08-19T06:49:36Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"title":"On the nature and physical conditions of the luminous Ly α emitter CR7 and its rest-frame UV components","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"abstract":[{"text":"We present new Hubble Space Telescope (HST)/WFC3 observations and re-analyse VLT data to unveil the continuum, variability, and rest-frame ultraviolet (UV) lines of the multiple UV clumps of the most luminous Lyα emitter at z = 6.6, CR7 (COSMOS Redshift 7). Our re-reduced, flux-calibrated X-SHOOTER spectra of CR7 reveal an He II emission line in observations obtained along the major axis of Lyα emission with the best seeing conditions. He II is spatially offset by ≈+0.8 arcsec from the peak of Lyα emission, and it is found towards clump B. Our WFC3 grism spectra detects the UV continuum of CR7’s clump A, yielding a power law with β=−2.5+0.6−0.7 and MUV=−21.87+0.25−0.20⁠. No significant variability is found for any of the UV clumps on their own, but there is tentative (≈2.2 σ) brightening of CR7 in F110W as a whole from 2012 to 2017. HST grism data fail to robustly detect rest-frame UV lines in any of the clumps, implying fluxes ≲2×10−17 erg s−1 cm−2 (3σ). We perform CLOUDY modelling to constrain the metallicity and the ionizing nature of CR7. CR7 seems to be actively forming stars without any clear active galactic nucleus activity in clump A, consistent with a metallicity of ∼0.05–0.2 Z⊙. Component C or an interclump component between B and C may host a high ionization source. Our results highlight the need for spatially resolved information to study the formation and assembly of early galaxies.","lang":"eng"}],"article_type":"original","publication_status":"published","date_published":"2019-01-01T00:00:00Z","volume":482,"oa":1,"year":"2019","arxiv":1,"month":"01","extern":"1","day":"01","oa_version":"Preprint","external_id":{"arxiv":["1710.08422"]},"intvolume":" 482","type":"journal_article","doi":"10.1093/mnras/sty2779","date_created":"2022-07-08T10:40:05Z","author":[{"full_name":"Sobral, David","first_name":"David","last_name":"Sobral"},{"id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","last_name":"Matthee"},{"first_name":"Gabriel","last_name":"Brammer","full_name":"Brammer, Gabriel"},{"last_name":"Ferrara","first_name":"Andrea","full_name":"Ferrara, Andrea"},{"last_name":"Alegre","first_name":"Lara","full_name":"Alegre, Lara"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Schaerer, Daniel","last_name":"Schaerer","first_name":"Daniel"},{"full_name":"Mobasher, Bahram","first_name":"Bahram","last_name":"Mobasher"},{"last_name":"Darvish","first_name":"Behnam","full_name":"Darvish, Behnam"}],"publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1710.08422"}],"_id":"11541"},{"issue":"4","page":"5616-5630","citation":{"apa":"Hon, M., Stello, D., García, R. A., Mathur, S., Sharma, S., Colman, I. L., & Bugnet, L. A. (2019). A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz622","ama":"Hon M, Stello D, García RA, et al. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 2019;485(4):5616-5630. doi:10.1093/mnras/stz622","ieee":"M. Hon et al., “A search for red giant solar-like oscillations in all Kepler data,” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4. Oxford University Press, pp. 5616–5630, 2019.","short":"M. Hon, D. Stello, R.A. García, S. Mathur, S. Sharma, I.L. Colman, L.A. Bugnet, Monthly Notices of the Royal Astronomical Society 485 (2019) 5616–5630.","chicago":"Hon, Marc, Dennis Stello, Rafael A García, Savita Mathur, Sanjib Sharma, Isabel L Colman, and Lisa Annabelle Bugnet. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz622.","ista":"Hon M, Stello D, García RA, Mathur S, Sharma S, Colman IL, Bugnet LA. 2019. A search for red giant solar-like oscillations in all Kepler data. Monthly Notices of the Royal Astronomical Society. 485(4), 5616–5630.","mla":"Hon, Marc, et al. “A Search for Red Giant Solar-like Oscillations in All Kepler Data.” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 4, Oxford University Press, 2019, pp. 5616–30, doi:10.1093/mnras/stz622."},"publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","methods: data analysis","techniques: image processing","stars: oscillations","stars: statistics"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","article_processing_charge":"No","title":"A search for red giant solar-like oscillations in all Kepler data","acknowledgement":"Funding for this Discovery mission is provided by NASA’s Science mission Directorate. We thank the entire Kepler team without whom this investigation would not be possible. DS is the recipient of an Australian Research Council Future Fellowship (project number FT1400147). RAG acknowledges the support from CNES. SM acknowledges support from NASA grant NNX15AF13G, NSF grant AST-1411685, and the Ramon y Cajal fellowship number RYC-2015-17697. ILC acknowledges scholarship support from the University of Sydney. We would like to thank Nicholas Barbara and Timothy Bedding for providing us with a list of variable stars that helped to validate a number of detections in this study. We also thank the group at the University of Sydney for fruitful discussions. Finally, we gratefully acknowledge the support of NVIDIA Corporation with the donation of the Titan Xp GPU used for this research.","date_updated":"2022-08-22T07:35:19Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"month":"06","extern":"1","oa_version":"Preprint","external_id":{"arxiv":["1903.00115"]},"day":"01","abstract":[{"lang":"eng","text":"The recently published Kepler mission Data Release 25 (DR25) reported on ∼197 000 targets observed during the mission. Despite this, no wide search for red giants showing solar-like oscillations have been made across all stars observed in Kepler’s long-cadence mode. In this work, we perform this task using custom apertures on the Kepler pixel files and detect oscillations in 21 914 stars, representing the largest sample of solar-like oscillating stars to date. We measure their frequency at maximum power, νmax, down to νmax≃4μHz and obtain log (g) estimates with a typical uncertainty below 0.05 dex, which is superior to typical measurements from spectroscopy. Additionally, the νmax distribution of our detections show good agreement with results from a simulated model of the Milky Way, with a ratio of observed to predicted stars of 0.992 for stars with 10<νmax<270μHz. Among our red giant detections, we find 909 to be dwarf/subgiant stars whose flux signal is polluted by a neighbouring giant as a result of using larger photometric apertures than those used by the NASA Kepler science processing pipeline. We further find that only 293 of the polluting giants are known Kepler targets. The remainder comprises over 600 newly identified oscillating red giants, with many expected to belong to the Galactic halo, serendipitously falling within the Kepler pixel files of targeted stars."}],"article_type":"original","publication_status":"published","arxiv":1,"volume":485,"date_published":"2019-06-01T00:00:00Z","oa":1,"year":"2019","_id":"11615","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1903.00115"}],"type":"journal_article","intvolume":" 485","date_created":"2022-07-18T14:26:03Z","author":[{"last_name":"Hon","first_name":"Marc","full_name":"Hon, Marc"},{"full_name":"Stello, Dennis","last_name":"Stello","first_name":"Dennis"},{"full_name":"García, Rafael A","last_name":"García","first_name":"Rafael A"},{"first_name":"Savita","last_name":"Mathur","full_name":"Mathur, Savita"},{"last_name":"Sharma","first_name":"Sanjib","full_name":"Sharma, Sanjib"},{"full_name":"Colman, Isabel L","first_name":"Isabel L","last_name":"Colman"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","orcid":"0000-0003-0142-4000","first_name":"Lisa Annabelle","last_name":"Bugnet"}],"doi":"10.1093/mnras/stz622"},{"article_type":"original","publication_status":"published","abstract":[{"text":"Weak lensing surveys are reaching sensitivities at which uncertainties in the galaxy redshift distributions n(z) from photo-z errors degrade cosmological constraints. We use ray-tracing simulations and a simple treatment of photo-z errors to assess cosmological parameter biases from uncertainties in n(z) in an LSST-like survey. We use lensing peak counts and the power spectrum to infer cosmological parameters, and find that the latter is somewhat more resilient to photo-z errors. We place conservative lower limits on the survey size at which different types of photo-z errors significantly degrade (${\\sim }50{{\\ \\rm per\\ cent}}$) ΛCDM (cold dark matter, wCDM) parameter constraints. A residual constant photo-z bias of |δz| &lt; 0.003(1 + z), the current LSST requirement, does not significantly degrade surveys smaller than ≈1300 (≈490) deg2 using peaks and ≈6500 (≈4900) deg2 using the power spectrum. Surveys smaller than ≈920 (≈450) deg2 and ≈4600 (≈4000) deg2 avoid 25 per cent degradation. Adopting a recent prediction for LSST’s full photo-z probability distribution function (PDF), we find that simply approximating n(z) with the photo-z galaxy distribution computed from this PDF significantly degrades surveys as small as ≈60 (≈65) deg2 using peaks or the power spectrum. If the centroid bias in each tomographic bin is removed from the photo-z galaxy distribution, using peaks or the power spectrum still significantly degrades surveys larger than ≈200 (≈255) or ≈248 (≈315) deg2; 25 per cent degradations occur at survey sizes of ≈140 (≈180) deg2 or ≈165 (≈210) deg2. These results imply that the expected broad photo-z PDF significantly biases parameters, which must be further mitigated using more sophisticated photo-z treatments.","lang":"eng"}],"year":"2019","oa":1,"volume":486,"date_published":"2019-04-18T00:00:00Z","extern":"1","month":"04","oa_version":"Published Version","day":"18","intvolume":" 486","type":"journal_article","author":[{"full_name":"Abruzzo, Matthew W","first_name":"Matthew W","last_name":"Abruzzo"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"}],"date_created":"2024-09-05T08:49:24Z","doi":"10.1093/mnras/stz1016","_id":"17510","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stz1016"}],"publication":"Monthly Notices of the Royal Astronomical Society","page":"2730-2753","citation":{"short":"M.W. Abruzzo, Z. Haiman, Monthly Notices of the Royal Astronomical Society 486 (2019) 2730–2753.","ista":"Abruzzo MW, Haiman Z. 2019. The impact of photometric redshift errors on lensing statistics in ray-tracing simulations. Monthly Notices of the Royal Astronomical Society. 486(2), 2730–2753.","mla":"Abruzzo, Matthew W., and Zoltán Haiman. “The Impact of Photometric Redshift Errors on Lensing Statistics in Ray-Tracing Simulations.” Monthly Notices of the Royal Astronomical Society, vol. 486, no. 2, Oxford University Press, 2019, pp. 2730–53, doi:10.1093/mnras/stz1016.","chicago":"Abruzzo, Matthew W, and Zoltán Haiman. “The Impact of Photometric Redshift Errors on Lensing Statistics in Ray-Tracing Simulations.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz1016.","ieee":"M. W. Abruzzo and Z. Haiman, “The impact of photometric redshift errors on lensing statistics in ray-tracing simulations,” Monthly Notices of the Royal Astronomical Society, vol. 486, no. 2. Oxford University Press, pp. 2730–2753, 2019.","ama":"Abruzzo MW, Haiman Z. The impact of photometric redshift errors on lensing statistics in ray-tracing simulations. Monthly Notices of the Royal Astronomical Society. 2019;486(2):2730-2753. doi:10.1093/mnras/stz1016","apa":"Abruzzo, M. W., & Haiman, Z. (2019). The impact of photometric redshift errors on lensing statistics in ray-tracing simulations. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz1016"},"scopus_import":"1","status":"public","issue":"2","article_processing_charge":"No","title":"The impact of photometric redshift errors on lensing statistics in ray-tracing simulations","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_updated":"2024-09-10T12:49:04Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"quality_controlled":"1"},{"article_processing_charge":"No","title":"Localization of binary black hole mergers with known inclination","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_updated":"2024-09-10T13:26:28Z","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"quality_controlled":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"4459-4463","citation":{"ieee":"K. R. Corley et al., “Localization of binary black hole mergers with known inclination,” Monthly Notices of the Royal Astronomical Society, vol. 488, no. 3. Oxford University Press, pp. 4459–4463, 2019.","ama":"Corley KR, Bartos I, Singer LP, et al. Localization of binary black hole mergers with known inclination. Monthly Notices of the Royal Astronomical Society. 2019;488(3):4459-4463. doi:10.1093/mnras/stz2072","apa":"Corley, K. R., Bartos, I., Singer, L. P., Williamson, A. R., Haiman, Z., Kocsis, B., … Márka, S. (2019). Localization of binary black hole mergers with known inclination. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2072","ista":"Corley KR, Bartos I, Singer LP, Williamson AR, Haiman Z, Kocsis B, Nissanke S, Márka Z, Márka S. 2019. Localization of binary black hole mergers with known inclination. Monthly Notices of the Royal Astronomical Society. 488(3), 4459–4463.","mla":"Corley, K. Rainer, et al. “Localization of Binary Black Hole Mergers with Known Inclination.” Monthly Notices of the Royal Astronomical Society, vol. 488, no. 3, Oxford University Press, 2019, pp. 4459–63, doi:10.1093/mnras/stz2072.","chicago":"Corley, K Rainer, Imre Bartos, Leo P Singer, Andrew R Williamson, Zoltán Haiman, Bence Kocsis, Samaya Nissanke, Zsuzsa Márka, and Szabolcs Márka. “Localization of Binary Black Hole Mergers with Known Inclination.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz2072.","short":"K.R. Corley, I. Bartos, L.P. Singer, A.R. Williamson, Z. Haiman, B. Kocsis, S. Nissanke, Z. Márka, S. Márka, Monthly Notices of the Royal Astronomical Society 488 (2019) 4459–4463."},"scopus_import":"1","status":"public","issue":"3","type":"journal_article","intvolume":" 488","date_created":"2024-09-05T08:51:22Z","author":[{"full_name":"Corley, K Rainer","last_name":"Corley","first_name":"K Rainer"},{"last_name":"Bartos","first_name":"Imre","full_name":"Bartos, Imre"},{"last_name":"Singer","first_name":"Leo P","full_name":"Singer, Leo P"},{"full_name":"Williamson, Andrew R","last_name":"Williamson","first_name":"Andrew R"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","first_name":"Zoltán","last_name":"Haiman"},{"first_name":"Bence","last_name":"Kocsis","full_name":"Kocsis, Bence"},{"full_name":"Nissanke, Samaya","first_name":"Samaya","last_name":"Nissanke"},{"full_name":"Márka, Zsuzsa","first_name":"Zsuzsa","last_name":"Márka"},{"last_name":"Márka","first_name":"Szabolcs","full_name":"Márka, Szabolcs"}],"doi":"10.1093/mnras/stz2072","_id":"17512","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stz2072"}],"article_type":"original","publication_status":"published","abstract":[{"lang":"eng","text":"The localization of stellar-mass binary black hole mergers using gravitational waves is critical in understanding the properties of the binaries’ host galaxies, observing possible electromagnetic emission from the mergers, or using them as a cosmological distance ladder. The precision of this localization can be substantially increased with prior astrophysical information about the binary system. In particular, constraining the inclination of the binary can reduce the distance uncertainty of the source. Here, we present the first realistic set of localizations for binary black hole mergers, including different prior constraints on the binaries’ inclinations. We find that prior information on the inclination can reduce the localization volume by a factor of 3. We discuss two astrophysical scenarios of interest: (i) follow-up searches for beamed electromagnetic/neutrino counterparts and (ii) mergers in the accretion discs of active galactic nuclei."}],"oa":1,"year":"2019","volume":488,"date_published":"2019-07-30T00:00:00Z","extern":"1","month":"07","oa_version":"Published Version","day":"30"},{"issue":"4","status":"public","scopus_import":"1","citation":{"ieee":"T. Lu and Z. Haiman, “The matter fluctuation amplitude inferred from the weak lensing power spectrum and correlation function in CFHTLenS data,” Monthly Notices of the Royal Astronomical Society, vol. 490, no. 4. Oxford University Press, pp. 5033–5042, 2019.","ama":"Lu T, Haiman Z. The matter fluctuation amplitude inferred from the weak lensing power spectrum and correlation function in CFHTLenS data. Monthly Notices of the Royal Astronomical Society. 2019;490(4):5033-5042. doi:10.1093/mnras/stz2931","apa":"Lu, T., & Haiman, Z. (2019). The matter fluctuation amplitude inferred from the weak lensing power spectrum and correlation function in CFHTLenS data. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2931","short":"T. Lu, Z. Haiman, Monthly Notices of the Royal Astronomical Society 490 (2019) 5033–5042.","mla":"Lu, Tianhuan, and Zoltán Haiman. “The Matter Fluctuation Amplitude Inferred from the Weak Lensing Power Spectrum and Correlation Function in CFHTLenS Data.” Monthly Notices of the Royal Astronomical Society, vol. 490, no. 4, Oxford University Press, 2019, pp. 5033–42, doi:10.1093/mnras/stz2931.","ista":"Lu T, Haiman Z. 2019. The matter fluctuation amplitude inferred from the weak lensing power spectrum and correlation function in CFHTLenS data. Monthly Notices of the Royal Astronomical Society. 490(4), 5033–5042.","chicago":"Lu, Tianhuan, and Zoltán Haiman. “The Matter Fluctuation Amplitude Inferred from the Weak Lensing Power Spectrum and Correlation Function in CFHTLenS Data.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz2931."},"page":"5033-5042","publication":"Monthly Notices of the Royal Astronomical Society","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","date_updated":"2024-09-11T08:01:58Z","publication_identifier":{"issn":["0035-8711","1365-2966"]},"title":"The matter fluctuation amplitude inferred from the weak lensing power spectrum and correlation function in CFHTLenS data","article_processing_charge":"No","day":"18","oa_version":"Published Version","extern":"1","month":"10","volume":490,"date_published":"2019-10-18T00:00:00Z","year":"2019","oa":1,"abstract":[{"text":"Based on the cosmic shear data from the Canada-France-Hawaii Telescope Lensing Survey (CFHTLenS), Kilbinger et al. (2013) obtained a constraint on the amplitude of matter fluctuations of σ8(Ωm/0.27)0.6=0.79±0.03 from the two-point correlation function (2PCF). This is ≈3σ lower than the value 0.89±0.01 derived from Planck data on cosmic microwave background (CMB) anisotropies. On the other hand, based on the same CFHTLenS data, but using the power spectrum, and performing a different analysis, Liu et al. (2015) obtained the higher value of σ8(Ωm/0.27)0.64=0.87+0.05−0.06. We here investigate the origin of this difference, by performing a fair side-by-side comparison of the 2PCF and power spectrum analyses on CFHTLenS data. We find that these two statistics indeed deliver different results, even when applied to the same data in an otherwise identical procedure. We identify excess power in the data on small scales (ℓ>5,000) driving the larger values inferred from the power spectrum. We speculate on the possible origin of this excess small-scale power. More generally, our results highlight the utility of analysing the 2PCF and the power spectrum in tandem, to discover (and to help control) systematic errors.","lang":"eng"}],"article_type":"original","publication_status":"published","related_material":{"link":[{"relation":"erratum","url":"https://doi.org/10.1093/mnras/stad1748"}]},"main_file_link":[{"url":"https://doi.org/10.1093/mnras/stz2931","open_access":"1"}],"publisher":"Oxford University Press","_id":"17530","doi":"10.1093/mnras/stz2931","author":[{"full_name":"Lu, Tianhuan","last_name":"Lu","first_name":"Tianhuan"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","last_name":"Haiman","first_name":"Zoltán"}],"date_created":"2024-09-05T09:37:20Z","intvolume":" 490","type":"journal_article"},{"doi":"10.1093/mnras/stz150","date_created":"2024-09-05T09:59:54Z","author":[{"full_name":"Kelley, Luke Zoltan","first_name":"Luke Zoltan","last_name":"Kelley"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán"},{"last_name":"Sesana","first_name":"Alberto","full_name":"Sesana, Alberto"},{"last_name":"Hernquist","first_name":"Lars","full_name":"Hernquist, Lars"}],"type":"journal_article","intvolume":" 485","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stz150","open_access":"1"}],"publisher":"Oxford University Press","_id":"17543","oa":1,"year":"2019","volume":485,"date_published":"2019-01-30T00:00:00Z","article_type":"original","publication_status":"published","abstract":[{"lang":"eng","text":"Massive black-hole (MBH) binaries, which are expected to form following the merger of their parent galaxies, produce gravitational waves which will be detectable by Pulsar Timing Arrays at nanohertz frequencies (year periods). While no confirmed, compact MBH binary systems have been seen in electromagnetic observations, a large number of candidates have recently been identified in optical surveys of AGN variability. Using a combination of cosmological, hydrodynamic simulations; comprehensive, semi-analytic binary merger models; and analytic AGN spectra and variability prescriptions; we calculate the expected electromagnetic detection rates of MBH binaries as periodically variable AGN. In particular, we consider two independent variability models: (i) Doppler boosting due to large orbital velocities, and (ii) hydrodynamic variability in which the fueling of MBH accretion disks is periodically modulated by the companion. Our models predict that numerous MBH binaries should be present and distinguishable in the existing data. In particular, our fiducial models produce an expectation value of 0.2 (Doppler) and 5 (hydrodynamic) binaries to be identifiable in CRTS, while 20 and 100 are expected after five years of LSST observations. The brightness variations in most systems are too small to be distinguishable, but almost 1% of AGN at redshifts z≲0.6 could be in massive binaries. We analyze the predicted binary parameters of observable systems and their selection biases, and include an extensive discussion of our model parameters and uncertainties."}],"day":"30","oa_version":"Published Version","extern":"1","month":"01","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_updated":"2024-09-18T08:52:07Z","title":"Massive BH binaries as periodically variable AGN","article_processing_charge":"No","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","status":"public","scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"ama":"Kelley LZ, Haiman Z, Sesana A, Hernquist L. Massive BH binaries as periodically variable AGN. Monthly Notices of the Royal Astronomical Society. 2019;485(2):1579-1594. doi:10.1093/mnras/stz150","apa":"Kelley, L. Z., Haiman, Z., Sesana, A., & Hernquist, L. (2019). Massive BH binaries as periodically variable AGN. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz150","ieee":"L. Z. Kelley, Z. Haiman, A. Sesana, and L. Hernquist, “Massive BH binaries as periodically variable AGN,” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 2. Oxford University Press, pp. 1579–1594, 2019.","short":"L.Z. Kelley, Z. Haiman, A. Sesana, L. Hernquist, Monthly Notices of the Royal Astronomical Society 485 (2019) 1579–1594.","chicago":"Kelley, Luke Zoltan, Zoltán Haiman, Alberto Sesana, and Lars Hernquist. “Massive BH Binaries as Periodically Variable AGN.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz150.","mla":"Kelley, Luke Zoltan, et al. “Massive BH Binaries as Periodically Variable AGN.” Monthly Notices of the Royal Astronomical Society, vol. 485, no. 2, Oxford University Press, 2019, pp. 1579–94, doi:10.1093/mnras/stz150.","ista":"Kelley LZ, Haiman Z, Sesana A, Hernquist L. 2019. Massive BH binaries as periodically variable AGN. Monthly Notices of the Royal Astronomical Society. 485(2), 1579–1594."},"page":"1579-1594","issue":"2"},{"status":"public","publication":"Monthly Notices of the Royal Astronomical Society","page":"2467-2473","citation":{"ieee":"J. Wolcott-Green and Z. Haiman, “H2 self-shielding with non-LTE rovibrational populations: Implications for cooling in protogalaxies,” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 2. Oxford University Press, pp. 2467–2473, 2019.","ama":"Wolcott-Green J, Haiman Z. H2 self-shielding with non-LTE rovibrational populations: Implications for cooling in protogalaxies. Monthly Notices of the Royal Astronomical Society. 2019;484(2):2467-2473. doi:10.1093/mnras/sty3280","apa":"Wolcott-Green, J., & Haiman, Z. (2019). H2 self-shielding with non-LTE rovibrational populations: Implications for cooling in protogalaxies. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty3280","short":"J. Wolcott-Green, Z. Haiman, Monthly Notices of the Royal Astronomical Society 484 (2019) 2467–2473.","mla":"Wolcott-Green, J., and Zoltán Haiman. “H2 Self-Shielding with Non-LTE Rovibrational Populations: Implications for Cooling in Protogalaxies.” Monthly Notices of the Royal Astronomical Society, vol. 484, no. 2, Oxford University Press, 2019, pp. 2467–73, doi:10.1093/mnras/sty3280.","ista":"Wolcott-Green J, Haiman Z. 2019. H2 self-shielding with non-LTE rovibrational populations: Implications for cooling in protogalaxies. Monthly Notices of the Royal Astronomical Society. 484(2), 2467–2473.","chicago":"Wolcott-Green, J, and Zoltán Haiman. “H2 Self-Shielding with Non-LTE Rovibrational Populations: Implications for Cooling in Protogalaxies.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/sty3280."},"scopus_import":"1","issue":"2","title":"H2 self-shielding with non-LTE rovibrational populations: Implications for cooling in protogalaxies","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_updated":"2024-09-18T12:00:29Z","article_processing_charge":"No","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"quality_controlled":"1","oa":1,"year":"2019","date_published":"2019-01-16T00:00:00Z","volume":484,"publication_status":"published","article_type":"original","abstract":[{"lang":"eng","text":"The abundance of molecular hydrogen (H2), the primary coolant in primordial gas, is critical for the thermodynamic evolution and star-formation histories in early protogalaxies. Determining the photodissociation rate of H2 by an incident Lyman-Werner (LW) flux is thus crucial, but prohibitively expensive to calculate on the fly in simulations. The rate is sensitive to the H2 rovibrational distribution, which in turn depends on the gas density, temperature, and incident LW radiation field. We use the publicly available cloudy package to model primordial gas clouds and compare exact photodissociation rate calculations to commonly-used fitting formulae. We find the fit from Wolcott-Green et al. (2011) is most accurate for moderate densities n~10^3 cm^{-3} and temperatures, T~10^3K, and we provide a new fit, which captures the increase in the rate at higher densities and temperatures, owing to the increased excited rovibrational populations in this regime. Our new fit has typical errors of a few percent percent up to n =<10^7 cm^{-3}, T =< 8000K, and H2 column density NH2 =<10^{17} cm^{-2}, and can be easily utilized in simulations. We also show that pumping of the excited rovibrational states of H2 by a strong LW flux further modifies the level populations when the gas density is low, and noticeably decreases self-shielding for J_21 > 10^3 and n < 10^2 cm^{-3}. This may lower the \"critical flux\" at which primordial gas remains H2-poor in some protogalaxies, enabling massive black hole seed formation."}],"oa_version":"Published Version","day":"16","month":"01","extern":"1","date_created":"2024-09-05T10:24:40Z","author":[{"full_name":"Wolcott-Green, J","first_name":"J","last_name":"Wolcott-Green"},{"first_name":"Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"}],"doi":"10.1093/mnras/sty3280","intvolume":" 484","type":"journal_article","_id":"17556","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/sty3280"}]},{"issue":"2","page":"2754-2765","citation":{"ieee":"A. M. Derdzinski, D. D’Orazio, P. Duffell, Z. Haiman, and A. MacFadyen, “Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc,” Monthly Notices of the Royal Astronomical Society, vol. 486, no. 2. Oxford University Press, pp. 2754–2765, 2019.","ama":"Derdzinski AM, D’Orazio D, Duffell P, Haiman Z, MacFadyen A. Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc. Monthly Notices of the Royal Astronomical Society. 2019;486(2):2754-2765. doi:10.1093/mnras/stz1026","apa":"Derdzinski, A. M., D’Orazio, D., Duffell, P., Haiman, Z., & MacFadyen, A. (2019). Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz1026","mla":"Derdzinski, A. M., et al. “Probing Gas Disc Physics with LISA: Simulations of an Intermediate Mass Ratio Inspiral in an Accretion Disc.” Monthly Notices of the Royal Astronomical Society, vol. 486, no. 2, Oxford University Press, 2019, pp. 2754–65, doi:10.1093/mnras/stz1026.","ista":"Derdzinski AM, D’Orazio D, Duffell P, Haiman Z, MacFadyen A. 2019. Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc. Monthly Notices of the Royal Astronomical Society. 486(2), 2754–2765.","chicago":"Derdzinski, A M, D D’Orazio, P Duffell, Zoltán Haiman, and A MacFadyen. “Probing Gas Disc Physics with LISA: Simulations of an Intermediate Mass Ratio Inspiral in an Accretion Disc.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz1026.","short":"A.M. Derdzinski, D. D’Orazio, P. Duffell, Z. Haiman, A. MacFadyen, Monthly Notices of the Royal Astronomical Society 486 (2019) 2754–2765."},"publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","status":"public","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"quality_controlled":"1","article_processing_charge":"No","title":"Probing gas disc physics with LISA: simulations of an intermediate mass ratio inspiral in an accretion disc","date_updated":"2024-09-18T11:01:36Z","publication_identifier":{"issn":["0035-8711","1365-2966"]},"extern":"1","month":"09","oa_version":"Published Version","day":"05","related_material":{"link":[{"url":"https://doi.org/10.1093/mnras/stz2435","relation":"erratum"}]},"abstract":[{"lang":"eng","text":"The coalescence of a compact object with a 104−107M⊙ supermassive black hole (SMBH) produces mHz gravitational waves (GWs) detectable by the future Laser Interferometer Space Antenna (LISA). If such an inspiral occurs in the accretion disc of an active galactic nucleus (AGN), the gas torques imprint a small deviation in the GW waveform. Here we present two-dimensional hydrodynamical simulations with the moving-mesh code DISCO of a BH inspiraling at the GW rate in a binary system with a mass ratio q=M2/M1=10−3, embedded in an accretion disc. We assume a locally isothermal equation of state for the gas (with Mach number M=20) and implement a standard α-prescription for its viscosity (with α=0.03). We find disc torques on the binary that are weaker than in previous semi-analytic toy models, and are in the opposite direction: the gas disc slows down, rather than speeds up the inspiral. We compute the resulting deviations in the GW waveform, which scale linearly with the mass of the disc. The SNR of these deviations accumulates mostly at high frequencies, and becomes detectable in a 5-year LISA observation if the total phase shift exceeds a few radians. We find that this occurs if the disc surface density exceeds Σ0≳102−3gcm−2, as may be the case in thin discs with near-Eddington accretion rates. Since the characteristic imprint on the GW signal is strongly dependent on disc parameters, a LISA detection of an intermediate mass ratio inspiral would probe the physics of AGN discs and migration."}],"publication_status":"published","article_type":"original","volume":486,"date_published":"2019-09-05T00:00:00Z","year":"2019","oa":1,"_id":"17565","main_file_link":[{"url":"https://doi.org/10.1093/mnras/stz1026","open_access":"1"}],"publisher":"Oxford University Press","intvolume":" 486","type":"journal_article","date_created":"2024-09-05T12:05:43Z","author":[{"first_name":"A M","last_name":"Derdzinski","full_name":"Derdzinski, A M"},{"full_name":"D’Orazio, D","last_name":"D’Orazio","first_name":"D"},{"full_name":"Duffell, P","last_name":"Duffell","first_name":"P"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"full_name":"MacFadyen, A","last_name":"MacFadyen","first_name":"A"}],"doi":"10.1093/mnras/stz1026"},{"type":"journal_article","intvolume":" 490","date_created":"2024-09-05T13:11:16Z","author":[{"full_name":"Ribli, Dezső","first_name":"Dezső","last_name":"Ribli"},{"full_name":"Pataki, Bálint Ármin","last_name":"Pataki","first_name":"Bálint Ármin"},{"first_name":"José Manuel","last_name":"Zorrilla Matilla","full_name":"Zorrilla Matilla, José Manuel"},{"full_name":"Hsu, Daniel","last_name":"Hsu","first_name":"Daniel"},{"first_name":"Zoltán","last_name":"Haiman","full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Csabai, István","last_name":"Csabai","first_name":"István"}],"doi":"10.1093/mnras/stz2610","_id":"17603","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1902.03663"}],"publisher":"Oxford University Press","abstract":[{"lang":"eng","text":"Weak gravitational lensing is one of the most promising cosmological probes of the late universe. Several large ongoing (DES, KiDS, HSC) and planned (LSST, Euclid, WFIRST) astronomical surveys attempt to collect even deeper and larger scale data on weak lensing. Due to gravitational collapse, the distribution of dark matter is non-Gaussian on small scales. However, observations are typically evaluated through the two-point correlation function of galaxy shear, which does not capture non-Gaussian features of the lensing maps. Previous studies attempted to extract non-Gaussian information from weak lensing observations through several higher order statistics such as the three-point correlation function, peak counts, or Minkowski functionals. Deep convolutional neural networks (CNN) emerged in the field of computer vision with tremendous success, and they offer a new and very promising framework to extract information from 2D or 3D astronomical data sets, confirmed by recent studies on weak lensing. We show that a CNN is able to yield significantly stricter constraints of (σ8, Ωm) cosmological parameters than the power spectrum using convergence maps generated by full N-body simulations and ray-tracing, at angular scales and shape noise levels relevant for future observations. In a scenario mimicking LSST or Euclid, the CNN yields 2.4–2.8 times smaller credible contours than the power spectrum, and 3.5–4.2 times smaller at noise levels corresponding to a deep space survey such as WFIRST. We also show that at shape noise levels achievable in future space surveys the CNN yields 1.4–2.1 times smaller contours than peak counts, a higher order statistic capable of extracting non-Gaussian information from weak lensing maps."}],"article_type":"original","publication_status":"published","arxiv":1,"date_published":"2019-09-17T00:00:00Z","volume":490,"oa":1,"year":"2019","month":"09","extern":"1","oa_version":"Preprint","external_id":{"arxiv":["1902.03663"]},"day":"17","article_processing_charge":"No","title":"Weak lensing cosmology with convolutional neural networks on noisy data","date_updated":"2024-09-23T13:50:39Z","publication_identifier":{"issn":["0035-8711","1365-2966"]},"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"quality_controlled":"1","citation":{"short":"D. Ribli, B.Á. Pataki, J.M. Zorrilla Matilla, D. Hsu, Z. Haiman, I. Csabai, Monthly Notices of the Royal Astronomical Society 490 (2019) 1843–1860.","chicago":"Ribli, Dezső, Bálint Ármin Pataki, José Manuel Zorrilla Matilla, Daniel Hsu, Zoltán Haiman, and István Csabai. “Weak Lensing Cosmology with Convolutional Neural Networks on Noisy Data.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2019. https://doi.org/10.1093/mnras/stz2610.","mla":"Ribli, Dezső, et al. “Weak Lensing Cosmology with Convolutional Neural Networks on Noisy Data.” Monthly Notices of the Royal Astronomical Society, vol. 490, no. 2, Oxford University Press, 2019, pp. 1843–60, doi:10.1093/mnras/stz2610.","ista":"Ribli D, Pataki BÁ, Zorrilla Matilla JM, Hsu D, Haiman Z, Csabai I. 2019. Weak lensing cosmology with convolutional neural networks on noisy data. Monthly Notices of the Royal Astronomical Society. 490(2), 1843–1860.","ama":"Ribli D, Pataki BÁ, Zorrilla Matilla JM, Hsu D, Haiman Z, Csabai I. Weak lensing cosmology with convolutional neural networks on noisy data. Monthly Notices of the Royal Astronomical Society. 2019;490(2):1843-1860. doi:10.1093/mnras/stz2610","apa":"Ribli, D., Pataki, B. Á., Zorrilla Matilla, J. M., Hsu, D., Haiman, Z., & Csabai, I. (2019). Weak lensing cosmology with convolutional neural networks on noisy data. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stz2610","ieee":"D. Ribli, B. Á. Pataki, J. M. Zorrilla Matilla, D. Hsu, Z. Haiman, and I. Csabai, “Weak lensing cosmology with convolutional neural networks on noisy data,” Monthly Notices of the Royal Astronomical Society, vol. 490, no. 2. Oxford University Press, pp. 1843–1860, 2019."},"page":"1843-1860","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","status":"public","issue":"2"},{"doi":"10.1093/mnras/sty925","author":[{"full_name":"Khostovan, A A","last_name":"Khostovan","first_name":"A A"},{"last_name":"Sobral","first_name":"D","full_name":"Sobral, D"},{"full_name":"Mobasher, B","last_name":"Mobasher","first_name":"B"},{"full_name":"Best, P N","last_name":"Best","first_name":"P N"},{"last_name":"Smail","first_name":"I","full_name":"Smail, I"},{"last_name":"Matthee","first_name":"Jorryt J","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J"},{"full_name":"Darvish, B","first_name":"B","last_name":"Darvish"},{"last_name":"Nayyeri","first_name":"H","full_name":"Nayyeri, H"},{"full_name":"Hemmati, S","first_name":"S","last_name":"Hemmati"},{"last_name":"Stott","first_name":"J P","full_name":"Stott, J P"}],"date_created":"2022-07-08T11:48:48Z","intvolume":" 478","type":"journal_article","main_file_link":[{"url":"https://arxiv.org/abs/1705.01101"}],"publisher":"Oxford University Press","_id":"11549","year":"2018","date_published":"2018-08-01T00:00:00Z","volume":478,"arxiv":1,"article_type":"original","publication_status":"published","abstract":[{"lang":"eng","text":"We investigate the clustering properties of ∼7000 H β + [O III] and [O II] narrowband-selected emitters at z ∼ 0.8–4.7 from the High-z Emission Line Survey. We find clustering lengths, r0, of 1.5–4.0 h−1 Mpc and minimum dark matter halo masses of 1010.7–12.1 M⊙ for our z = 0.8–3.2 H β + [O III] emitters and r0 ∼ 2.0–8.3 h−1 Mpc and halo masses of 1011.5–12.6 M⊙ for our z = 1.5–4.7 [O II] emitters. We find r0 to strongly increase both with increasing line luminosity and redshift. By taking into account the evolution of the characteristic line luminosity, L⋆(z), and using our model predictions of halo mass given r0, we find a strong, redshift-independent increasing trend between L/L⋆(z) and minimum halo mass. The faintest H β + [O III] emitters are found to reside in 109.5 M⊙ haloes and the brightest emitters in 1013.0 M⊙ haloes. For [O II] emitters, the faintest emitters are found in 1010.5 M⊙ haloes and the brightest emitters in 1012.6 M⊙ haloes. A redshift-independent stellar mass dependency is also observed where the halo mass increases from 1011 to 1012.5 M⊙ for stellar masses of 108.5 to 1011.5 M⊙, respectively. We investigate the interdependencies of these trends by repeating our analysis in a Lline−Mstar grid space for our most populated samples (H β + [O III] z = 0.84 and [O II] z = 1.47) and find that the line luminosity dependency is stronger than the stellar mass dependency on halo mass. For L > L⋆ emitters at all epochs, we find a relatively flat trend with halo masses of 1012.5–13 M⊙, which may be due to quenching mechanisms in massive haloes that is consistent with a transitional halo mass predicted by models."}],"day":"01","external_id":{"arxiv":["1705.01101"]},"oa_version":"Published Version","month":"08","extern":"1","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"acknowledgement":"We thank the anonymous referee for their useful comments and suggestions that improved this study. AAK thanks Anahita Alavi and Irene Shivaei for useful discussion in the making of this paper. AAK acknowledges that this work was supported by NASA Headquarters under the NASA Earth and Space Science Fellowship Program – Grant NNX16AO92H. DS acknowledges financial support from the Netherlands Organization for Scientific Research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. PNB is grateful for support from STFC via grant STM001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Grant DUSTYGAL (321334), and a Royal Society/Wolfson Merit award. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G.","date_updated":"2022-08-19T06:53:39Z","title":"The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass","article_processing_charge":"No","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: star formation","cosmology: observations","large-scale structure of Universe"],"status":"public","scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"2999-3015","citation":{"ieee":"A. A. Khostovan et al., “The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 3. Oxford University Press, pp. 2999–3015, 2018.","apa":"Khostovan, A. A., Sobral, D., Mobasher, B., Best, P. N., Smail, I., Matthee, J. J., … Stott, J. P. (2018). The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty925","ama":"Khostovan AA, Sobral D, Mobasher B, et al. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 2018;478(3):2999-3015. doi:10.1093/mnras/sty925","short":"A.A. Khostovan, D. Sobral, B. Mobasher, P.N. Best, I. Smail, J.J. Matthee, B. Darvish, H. Nayyeri, S. Hemmati, J.P. Stott, Monthly Notices of the Royal Astronomical Society 478 (2018) 2999–3015.","mla":"Khostovan, A. A., et al. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 3, Oxford University Press, 2018, pp. 2999–3015, doi:10.1093/mnras/sty925.","ista":"Khostovan AA, Sobral D, Mobasher B, Best PN, Smail I, Matthee JJ, Darvish B, Nayyeri H, Hemmati S, Stott JP. 2018. The clustering of H β + [O III] and [O II] emitters since z ∼ 5: Dependencies with line luminosity and stellar mass. Monthly Notices of the Royal Astronomical Society. 478(3), 2999–3015.","chicago":"Khostovan, A A, D Sobral, B Mobasher, P N Best, I Smail, Jorryt J Matthee, B Darvish, H Nayyeri, S Hemmati, and J P Stott. “The Clustering of H β + [O III] and [O II] Emitters since z ∼ 5: Dependencies with Line Luminosity and Stellar Mass.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty925."},"issue":"3"},{"oa_version":"Preprint","external_id":{"arxiv":["1712.03985"]},"day":"01","extern":"1","month":"07","arxiv":1,"date_published":"2018-07-01T00:00:00Z","volume":478,"year":"2018","oa":1,"abstract":[{"text":"We investigate the morphology of the [C II] emission in a sample of ‘normal’ star-forming galaxies at 5 < z < 7.2 in relation to their UV (rest-frame) counterpart. We use new Atacama Large Millimetre/submillimetre Array (ALMA) observations of galaxies at z ∼ 6–7, as well as a careful re-analysis of archival ALMA data. In total 29 galaxies were analysed, 21 of which are detected in [C II]. For several of the latter the [C II] emission breaks into multiple components. Only a fraction of these [C II] components, if any, is associated with the primary UV systems, while the bulk of the [C II] emission is associated either with fainter UV components, or not associated with any UV counterpart at the current limits. By taking into account the presence of all these components, we find that the L[CII]–SFR (star formation rate) relation at early epochs is fully consistent with the local relation, but it has a dispersion of 0.48 ± 0.07 dex, which is about two times larger than observed locally. We also find that the deviation from the local L[CII]–SFR relation has a weak anticorrelation with the EW(Ly α). The morphological analysis also reveals that [C II] emission is generally much more extended than the UV emission. As a consequence, these primordial galaxies are characterized by a [C II] surface brightness generally much lower than expected from the local Σ[CII]−ΣSFR relation. These properties are likely a consequence of a combination of different effects, namely gas metallicity, [C II] emission from obscured star-forming regions, strong variations of the ionization parameter, and circumgalactic gas in accretion or ejected by these primeval galaxies.","lang":"eng"}],"publication_status":"published","article_type":"original","_id":"11555","publisher":"Oxford University Press","main_file_link":[{"url":"https://arxiv.org/abs/1712.03985","open_access":"1"}],"author":[{"last_name":"Carniani","first_name":"S","full_name":"Carniani, S"},{"first_name":"R","last_name":"Maiolino","full_name":"Maiolino, R"},{"full_name":"Amorin, R","last_name":"Amorin","first_name":"R"},{"last_name":"Pentericci","first_name":"L","full_name":"Pentericci, L"},{"last_name":"Pallottini","first_name":"A","full_name":"Pallottini, A"},{"full_name":"Ferrara, A","last_name":"Ferrara","first_name":"A"},{"full_name":"Willott, C J","first_name":"C J","last_name":"Willott"},{"first_name":"R","last_name":"Smit","full_name":"Smit, R"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"full_name":"Sobral, D","last_name":"Sobral","first_name":"D"},{"full_name":"Santini, P","last_name":"Santini","first_name":"P"},{"full_name":"Castellano, M","first_name":"M","last_name":"Castellano"},{"full_name":"De Barros, S","last_name":"De Barros","first_name":"S"},{"full_name":"Fontana, A","first_name":"A","last_name":"Fontana"},{"full_name":"Grazian, A","first_name":"A","last_name":"Grazian"},{"full_name":"Guaita, L","first_name":"L","last_name":"Guaita"}],"date_created":"2022-07-11T08:05:42Z","doi":"10.1093/mnras/sty1088","intvolume":" 478","type":"journal_article","issue":"1","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: formation"],"page":"1170-1184","citation":{"chicago":"Carniani, S, R Maiolino, R Amorin, L Pentericci, A Pallottini, A Ferrara, C J Willott, et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty1088.","ista":"Carniani S, Maiolino R, Amorin R, Pentericci L, Pallottini A, Ferrara A, Willott CJ, Smit R, Matthee JJ, Sobral D, Santini P, Castellano M, De Barros S, Fontana A, Grazian A, Guaita L. 2018. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 478(1), 1170–1184.","mla":"Carniani, S., et al. “Kiloparsec-Scale Gaseous Clumps and Star Formation at z = 5–7.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1, Oxford University Press, 2018, pp. 1170–84, doi:10.1093/mnras/sty1088.","short":"S. Carniani, R. Maiolino, R. Amorin, L. Pentericci, A. Pallottini, A. Ferrara, C.J. Willott, R. Smit, J.J. Matthee, D. Sobral, P. Santini, M. Castellano, S. De Barros, A. Fontana, A. Grazian, L. Guaita, Monthly Notices of the Royal Astronomical Society 478 (2018) 1170–1184.","apa":"Carniani, S., Maiolino, R., Amorin, R., Pentericci, L., Pallottini, A., Ferrara, A., … Guaita, L. (2018). Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty1088","ama":"Carniani S, Maiolino R, Amorin R, et al. Kiloparsec-scale gaseous clumps and star formation at z = 5–7. Monthly Notices of the Royal Astronomical Society. 2018;478(1):1170-1184. doi:10.1093/mnras/sty1088","ieee":"S. Carniani et al., “Kiloparsec-scale gaseous clumps and star formation at z = 5–7,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 1. Oxford University Press, pp. 1170–1184, 2018."},"publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","title":"Kiloparsec-scale gaseous clumps and star formation at z = 5–7","acknowledgement":"This paper makes use of the following ALMA data:\r\nADS/JAO.ALMA#2012.1.00719.S, ADS/JAO.ALMA#2012.A.00040.S,\r\nADS/JAO.ALMA#2013.A.00433.S, ADS/JAO.ALMA#2011.0.00115.S,\r\nADS/JAO.ALMA#2012.1.00033.S, ADS/JAO.ALMA#2012.1.00523.S,\r\nADS/JAO.ALMA#2013.1.00815.S, ADS/JAO.ALMA#2015.1.00834.S.,\r\nADS/JAO.ALMA#2015.1.01105.S, AND ADS/JAO.ALMA#2016.1.01240.S\r\nwhich can be retrieved from the ALMA data archive:\r\nhttps://almascience.eso.org/ alma-data/archive. ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada) and NSC and ASIAA (Taiwan), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ. We are grateful to G. Jones to for providing his [C II] flux maps. RM and SC acknowledge support by the Science and Technology Facilities Council (STFC). RM acknowledges ERC Advanced Grant 695671 ‘QUENCH’. AF acknowledges support from the ERC Advanced Grant INTERSTELLAR H2020/740120.","date_updated":"2022-08-19T06:58:06Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"article_processing_charge":"No"},{"publication_status":"published","article_type":"original","abstract":[{"lang":"eng","text":"Deep narrow-band surveys have revealed a large population of faint Ly α emitters (LAEs) in the distant Universe, but relatively little is known about the most luminous sources (⁠LLyα≳1042.7 erg s−1; LLyα≳L∗Lyα⁠). Here we present the spectroscopic follow-up of 21 luminous LAEs at z ∼ 2–3 found with panoramic narrow-band surveys over five independent extragalactic fields (≈4 × 106 Mpc3 surveyed at z ∼ 2.2 and z ∼ 3.1). We use WHT/ISIS, Keck/DEIMOS, and VLT/X-SHOOTER to study these sources using high ionization UV lines. Luminous LAEs at z ∼ 2–3 have blue UV slopes (⁠β=−2.0+0.3−0.1⁠) and high Ly α escape fractions (⁠50+20−15 per cent) and span five orders of magnitude in UV luminosity (MUV ≈ −19 to −24). Many (70 per cent) show at least one high ionization rest-frame UV line such as C IV, N V, C III], He II or O III], typically blue-shifted by ≈100–200 km s−1 relative to Ly α. Their Ly α profiles reveal a wide variety of shapes, including significant blue-shifted components and widths from 200 to 4000 km s−1. Overall, 60 ± 11  per cent appear to be active galactic nucleus (AGN) dominated, and at LLyα > 1043.3 erg s−1 and/or MUV < −21.5 virtually all LAEs are AGNs with high ionization parameters (log U = 0.6 ± 0.5) and with metallicities of ≈0.5 − 1 Z⊙. Those lacking signatures of AGNs (40 ± 11  per cent) have lower ionization parameters (⁠logU=−3.0+1.6−0.9 and log ξion = 25.4 ± 0.2) and are apparently metal-poor sources likely powered by young, dust-poor ‘maximal’ starbursts. Our results show that luminous LAEs at z ∼ 2–3 are a diverse population and that 2×L∗Lyα and 2×M∗UV mark a sharp transition in the nature of LAEs, from star formation dominated to AGN dominated."}],"oa":1,"year":"2018","date_published":"2018-06-01T00:00:00Z","volume":477,"arxiv":1,"extern":"1","month":"06","day":"01","external_id":{"arxiv":["1802.10102"]},"oa_version":"Preprint","intvolume":" 477","type":"journal_article","doi":"10.1093/mnras/sty782","date_created":"2022-07-12T07:18:02Z","author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"first_name":"Philip N","last_name":"Best","full_name":"Best, Philip N"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"},{"last_name":"Röttgering","first_name":"Huub","full_name":"Röttgering, Huub"},{"full_name":"Mobasher, Bahram","last_name":"Mobasher","first_name":"Bahram"},{"full_name":"Paulino-Afonso, Ana","last_name":"Paulino-Afonso","first_name":"Ana"},{"full_name":"Stroe, Andra","first_name":"Andra","last_name":"Stroe"},{"last_name":"Oteo","first_name":"Iván","full_name":"Oteo, Iván"}],"publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1802.10102"}],"_id":"11557","scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"2817-2840","citation":{"short":"D. Sobral, J.J. Matthee, B. Darvish, I. Smail, P.N. Best, L. Alegre, H. Röttgering, B. Mobasher, A. Paulino-Afonso, A. Stroe, I. Oteo, Monthly Notices of the Royal Astronomical Society 477 (2018) 2817–2840.","mla":"Sobral, David, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal Astronomical Society, vol. 477, no. 2, Oxford University Press, 2018, pp. 2817–40, doi:10.1093/mnras/sty782.","ista":"Sobral D, Matthee JJ, Darvish B, Smail I, Best PN, Alegre L, Röttgering H, Mobasher B, Paulino-Afonso A, Stroe A, Oteo I. 2018. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 477(2), 2817–2840.","chicago":"Sobral, David, Jorryt J Matthee, Behnam Darvish, Ian Smail, Philip N Best, Lara Alegre, Huub Röttgering, et al. “The Nature of Luminous Ly α Emitters at z ∼ 2–3: Maximal Dust-Poor Starbursts and Highly Ionizing AGN.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty782.","ieee":"D. Sobral et al., “The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN,” Monthly Notices of the Royal Astronomical Society, vol. 477, no. 2. Oxford University Press, pp. 2817–2840, 2018.","ama":"Sobral D, Matthee JJ, Darvish B, et al. The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. 2018;477(2):2817-2840. doi:10.1093/mnras/sty782","apa":"Sobral, D., Matthee, J. J., Darvish, B., Smail, I., Best, P. N., Alegre, L., … Oteo, I. (2018). The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty782"},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: evolution","galaxies: high-redshift","galaxies: ISM","galaxies: starburst","cosmology: observations"],"status":"public","issue":"2","article_processing_charge":"No","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"acknowledgement":"We thank the anonymous reviewer for their timely and constructive comments that greatly helped us to improve the manuscript. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G, and the National Science Foundation, grant number 1716907. IRS acknowledges support from the ERC Advanced Grant DUSTYGAL (321334), STFC (ST/P000541/1), and a Royal Society/Wolfson Merit Award. PNB is grateful for support from STFC via grant ST/M001229/1. We thank Anne Verhamme, Kimihiko Nakajima, Ryan Trainor, Sangeeta Malhotra, Max Gronke, James Rhoads, Fang Xia An, Matthew Hayes, Takashi Kojima, Mark Dijkstra, and Anne Jaskot for many helpful and engaging discussions, particularly during the SnowCLAW Ly α workshop. We thank Bruno Ribeiro, Stephane Charlot, and Joseph Caruana for comments on the manuscript. The authors would also like to thank Ingrid Tengs, Meg Singleton, Ali Khostovan, and Sara Perez for participating in part of the observations. We also thank Joao Calhau, Leah Morabito, Sergio Santos, and Aayush Saxena for their assistance with the narrow-band observations which allowed to select some of the sour ces. Based on observations obtained with the William Herschel Telescope, program: W16AN004; the Very Large Telescope, programs: 098.A-0819 & 099.A-0254; and the Keck II telescope, program: C267D. Based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 294.A-5039, 092.A-0786, 093.A-0561, 097.A-0943, 098.A-0819, 099.A-0254 and 179.A-2005. The authors acknowledge the award of service time (SW2014b20) on the WHT. WHT and its service programme are operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. The authors would also like to thank all the extremely helpful observatory staff that have greatly contributed towards our observations, particularly Fiona Riddick, Lilian Dominguez, Florencia Jimenez, and Ian Skillen. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY & SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2013). This research has made use of the VizieR catalogue access tool, CDS, Strasbourg, France.","date_updated":"2022-08-19T07:01:08Z","title":"The nature of luminous Ly α emitters at z ∼ 2–3: Maximal dust-poor starbursts and highly ionizing AGN","quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"quality_controlled":"1","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_updated":"2022-08-19T07:04:45Z","acknowledgement":"We thank the anonymous referee for their constructive comments that helped us improve the manuscript. DS acknowledges the hospitality of the IAC and a Severo Ochoa visiting grant. SS and JC acknowledge studentships from the Lancaster University. JM acknowledges a Huygens PhD fellowship from Leiden University. APA acknowledges financial support from the Science and Technology Foundation (FCT, Portugal) through research grants UID/FIS/04434/2013 and fellowship PD/BD/52706/2014. The authors thank Alyssa Drake, Kimihiko Nakajima, Yuichi Harikane, Max Gronke, Irene Shivaei, Helmut Dannerbauer, Huub Rottgering, ¨ Marius Eide, and Masami Ouchi for many engaging and stimulating discussions. We also thank Sara Perez, Alex Bennett, and Tom Rose for their involvement in the early stages of this project. Based on data products from observations made with European Southern Observatory (ESO) Telescopes at the La Silla Paranal Observatory under ESO programme IDs 294.A-5018, 097.A 0943,\r\n098.A-0819, 099.A-0254, and 179.A-2005 and on data products produced by TERAPIX and the Cambridge Astronomy Survey Unit on behalf of the UltraVISTA consortium. Based on observations using the WFC on the 2.5 m INT, as part of programmes 2013AN002, 2013BN008, 2014AC88, 2014AN002, 2014BN006, 2014BC118, and 2016AN001. The INT is operated on the island of La Palma by the Isaac Newton Group in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias. This work is based in part on data products produced at TERAPIX available at the Canadian Astronomy Data Centre as part of the Canada–France– Hawaii Telescope Legacy Survey (CFHTLS), a collaborative project of NRC and CNRS.\r\nWe are grateful to the CFHTLS, COSMOS-UltraVISTA, and COSMOS survey teams. We are also unmeasurably thankful to the pioneering and continuous work from previous Ly α surveys’ teams. Without these previous Ly α and the wider reach legacy surveys, this research would have been impossible. We also thank the VUDS team for making available spectroscopic redshifts from data obtained with VIMOS at the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Programme 185.A-0791. Finally, the authors acknowledge the unique value of the publicly available programming language PYTHON, including the NUMPY and SCIPY (Van Der Walt, Colbert & Varoquaux 2011; Jones et al. 2001), MATPLOTLIB (Hunter 2007), ASTROPY (Astropy Collaboration et al. 2013), and the TOPCAT analysis program (Taylor 2005). We publicly release a catalogue with all LAEs used in this paper (SC4K), so it can be freely explored by the community (see five example entries in Table A1).","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"title":"Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6","article_processing_charge":"No","issue":"4","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics"],"scopus_import":"1","page":"4725-4752","citation":{"ama":"Sobral D, Santos S, Matthee JJ, et al. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 2018;476(4):4725-4752. doi:10.1093/mnras/sty378","apa":"Sobral, D., Santos, S., Matthee, J. J., Paulino-Afonso, A., Ribeiro, B., Calhau, J., & Khostovan, A. A. (2018). Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty378","ieee":"D. Sobral et al., “Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6,” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4. Oxford University Press, pp. 4725–4752, 2018.","short":"D. Sobral, S. Santos, J.J. Matthee, A. Paulino-Afonso, B. Ribeiro, J. Calhau, A.A. Khostovan, Monthly Notices of the Royal Astronomical Society 476 (2018) 4725–4752.","chicago":"Sobral, David, Sérgio Santos, Jorryt J Matthee, Ana Paulino-Afonso, Bruno Ribeiro, João Calhau, and Ali A Khostovan. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty378.","ista":"Sobral D, Santos S, Matthee JJ, Paulino-Afonso A, Ribeiro B, Calhau J, Khostovan AA. 2018. Slicing COSMOS with SC4K: The evolution of typical Ly α emitters and the Ly α escape fraction from z ∼ 2 to 6. Monthly Notices of the Royal Astronomical Society. 476(4), 4725–4752.","mla":"Sobral, David, et al. “Slicing COSMOS with SC4K: The Evolution of Typical Ly α Emitters and the Ly α Escape Fraction from z ∼ 2 to 6.” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4, Oxford University Press, 2018, pp. 4725–52, doi:10.1093/mnras/sty378."},"publication":"Monthly Notices of the Royal Astronomical Society","main_file_link":[{"url":"https://arxiv.org/abs/1712.04451","open_access":"1"}],"publisher":"Oxford University Press","_id":"11558","doi":"10.1093/mnras/sty378","date_created":"2022-07-12T10:41:08Z","author":[{"last_name":"Sobral","first_name":"David","full_name":"Sobral, David"},{"full_name":"Santos, Sérgio","last_name":"Santos","first_name":"Sérgio"},{"first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Paulino-Afonso","first_name":"Ana","full_name":"Paulino-Afonso, Ana"},{"last_name":"Ribeiro","first_name":"Bruno","full_name":"Ribeiro, Bruno"},{"full_name":"Calhau, João","last_name":"Calhau","first_name":"João"},{"full_name":"Khostovan, Ali A","first_name":"Ali A","last_name":"Khostovan"}],"type":"journal_article","intvolume":" 476","day":"01","oa_version":"Preprint","external_id":{"arxiv":["1712.04451"]},"extern":"1","month":"06","volume":476,"date_published":"2018-06-01T00:00:00Z","year":"2018","oa":1,"arxiv":1,"abstract":[{"lang":"eng","text":"We present and explore deep narrow- and medium-band data obtained with the Subaru and the Isaac Newton Telescopes in the ∼2 deg2 COSMOS field. We use these data as an extremely wide, low-resolution (R ∼ 20–80) Integral Field Unit survey to slice through the COSMOS field and obtain a large sample of ∼4000 Ly α emitters (LAEs) from z ∼ 2 to 6 in 16 redshift slices (SC4K). We present new Ly α luminosity functions (LFs) covering a comoving volume of ∼108 Mpc3. SC4K extensively complements ultradeep surveys, jointly covering over 4 dex in Ly α luminosity and revealing a global (2.5 < z < 6) synergy LF with α=−1.93+0.12−0.12⁠, log10Φ∗Lyα=−3.45+0.22−0.29 Mpc−3, and log10L∗Lyα=42.93+0.15−0.11 erg s−1. The Schechter component of the Ly α LF reveals a factor ∼5 rise in L∗Lyα and a ∼7 × decline in Φ∗Lyα from z ∼ 2 to 6. The data reveal an extra power-law (or Schechter) component above LLy α ≈ 1043.3 erg s−1 at z ∼ 2.2–3.5 and we show that it is partially driven by X-ray and radio active galactic nucleus (AGN), as their Ly α LF resembles the excess. The power-law component vanishes and/or is below our detection limits above z > 3.5, likely linked with the evolution of the AGN population. The Ly α luminosity density rises by a factor ∼2 from z ∼ 2 to 3 but is then found to be roughly constant (⁠1.1+0.2−0.2×1040 erg s−1 Mpc−3) to z ∼ 6, despite the ∼0.7 dex drop in ultraviolet (UV) luminosity density. The Ly α/UV luminosity density ratio rises from 4 ± 1 per cent to 30 ± 6 per cent from z ∼ 2.2 to 6. Our results imply a rise of a factor of ≈2 in the global ionization efficiency (ξion) and a factor ≈4 ± 1 in the Ly α escape fraction from z ∼ 2 to 6, hinting for evolution in both the typical burstiness/stellar populations and even more so in the typical interstellar medium conditions allowing Ly α photons to escape."}],"article_type":"original","publication_status":"published"},{"_id":"11620","main_file_link":[{"url":"https://arxiv.org/abs/1805.01860","open_access":"1"}],"publisher":"Oxford University Press","date_created":"2022-07-18T14:43:17Z","author":[{"first_name":"V","last_name":"Van Eylen","full_name":"Van Eylen, V"},{"last_name":"Dai","first_name":"F","full_name":"Dai, F"},{"first_name":"S","last_name":"Mathur","full_name":"Mathur, S"},{"full_name":"Gandolfi, D","first_name":"D","last_name":"Gandolfi"},{"last_name":"Albrecht","first_name":"S","full_name":"Albrecht, S"},{"full_name":"Fridlund, M","last_name":"Fridlund","first_name":"M"},{"full_name":"García, R A","first_name":"R A","last_name":"García"},{"full_name":"Guenther, E","first_name":"E","last_name":"Guenther"},{"full_name":"Hjorth, M","first_name":"M","last_name":"Hjorth"},{"full_name":"Justesen, A B","last_name":"Justesen","first_name":"A B"},{"full_name":"Livingston, J","first_name":"J","last_name":"Livingston"},{"first_name":"M N","last_name":"Lund","full_name":"Lund, M N"},{"full_name":"Pérez Hernández, F","last_name":"Pérez Hernández","first_name":"F"},{"full_name":"Prieto-Arranz, J","first_name":"J","last_name":"Prieto-Arranz"},{"full_name":"Regulo, C","first_name":"C","last_name":"Regulo"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","full_name":"Bugnet, Lisa Annabelle","last_name":"Bugnet","first_name":"Lisa Annabelle"},{"full_name":"Everett, M E","first_name":"M E","last_name":"Everett"},{"full_name":"Hirano, T","last_name":"Hirano","first_name":"T"},{"full_name":"Nespral, D","first_name":"D","last_name":"Nespral"},{"full_name":"Nowak, G","first_name":"G","last_name":"Nowak"},{"full_name":"Palle, E","first_name":"E","last_name":"Palle"},{"first_name":"V","last_name":"Silva Aguirre","full_name":"Silva Aguirre, V"},{"full_name":"Trifonov, T","last_name":"Trifonov","first_name":"T"},{"last_name":"Winn","first_name":"J N","full_name":"Winn, J N"},{"full_name":"Barragán, O","first_name":"O","last_name":"Barragán"},{"last_name":"Beck","first_name":"P G","full_name":"Beck, P G"},{"first_name":"W J","last_name":"Chaplin","full_name":"Chaplin, W J"},{"last_name":"Cochran","first_name":"W D","full_name":"Cochran, W D"},{"full_name":"Csizmadia, S","last_name":"Csizmadia","first_name":"S"},{"first_name":"H","last_name":"Deeg","full_name":"Deeg, H"},{"full_name":"Endl, M","first_name":"M","last_name":"Endl"},{"last_name":"Heeren","first_name":"P","full_name":"Heeren, P"},{"first_name":"S","last_name":"Grziwa","full_name":"Grziwa, S"},{"last_name":"Hatzes","first_name":"A P","full_name":"Hatzes, A P"},{"first_name":"D","last_name":"Hidalgo","full_name":"Hidalgo, D"},{"last_name":"Korth","first_name":"J","full_name":"Korth, J"},{"last_name":"Mathis","first_name":"S","full_name":"Mathis, S"},{"full_name":"Montañes Rodriguez, P","last_name":"Montañes Rodriguez","first_name":"P"},{"full_name":"Narita, N","last_name":"Narita","first_name":"N"},{"last_name":"Patzold","first_name":"M","full_name":"Patzold, M"},{"full_name":"Persson, C M","last_name":"Persson","first_name":"C M"},{"full_name":"Rodler, F","last_name":"Rodler","first_name":"F"},{"last_name":"Smith","first_name":"A M S","full_name":"Smith, A M S"}],"doi":"10.1093/mnras/sty1390","intvolume":" 478","type":"journal_article","oa_version":"Preprint","external_id":{"arxiv":["1805.01860"]},"day":"01","extern":"1","month":"08","arxiv":1,"volume":478,"date_published":"2018-08-01T00:00:00Z","oa":1,"year":"2018","abstract":[{"lang":"eng","text":"We report the discovery and characterization of HD 89345b (K2-234b; EPIC 248777106b), a Saturn-sized planet orbiting a slightly evolved star. HD 89345 is a bright star (V = 9.3 mag) observed by the K2 mission with 1 min time sampling. It exhibits solar-like oscillations. We conducted asteroseismology to determine the parameters of the star, finding the mass and radius to be 1.12+0.04−0.01M⊙ and 1.657+0.020−0.004R⊙⁠, respectively. The star appears to have recently left the main sequence, based on the inferred age, 9.4+0.4−1.3Gyr⁠, and the non-detection of mixed modes. The star hosts a ‘warm Saturn’ (P = 11.8 d, Rp = 6.86 ± 0.14 R⊕). Radial-velocity follow-up observations performed with the FIbre-fed Echelle Spectrograph, HARPS, and HARPS-N spectrographs show that the planet has a mass of 35.7 ± 3.3 M⊕. The data also show that the planet’s orbit is eccentric (e ≈ 0.2). An investigation of the rotational splitting of the oscillation frequencies of the star yields no conclusive evidence on the stellar inclination angle. We further obtained Rossiter–McLaughlin observations, which result in a broad posterior of the stellar obliquity. The planet seems to confirm to the same patterns that have been observed for other sub-Saturns regarding planet mass and multiplicity, orbital eccentricity, and stellar metallicity."}],"publication_status":"published","article_type":"original","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","title":"HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2","acknowledgement":"We gratefully acknowledge many helpful suggestions by the anonymous referee. Based on observations made with a) the Nordic Optical Telescope, operated by the Nordic Optical Telescope Scientific Association at the Observatorio del Roque de los Muchachos; b) the ESO-3.6m telescope at La Silla Observatory under programme ID 0100.C-0808; c) the Italian Telescopio Nazionale Galileo operated on the island of La Palma by the Fundación Galileo Galilei of the Istituto Nazionale di Astrofisica. NESSI was funded by the NASA Exoplanet Exploration Program and the NASA Ames Research Center. NESSI was built at the Ames Research Center by Steve B. Howell, Nic Scott, Elliott P. Horch, and Emmett Quigley. This project has received funding from the European Union’s Horizon 2020 research and innovation programme under grant agreement No 730890. This material reflects only the authors views and the Commission is not liable for any use that may be made of the information contained therein. DG gratefully acknowledges the financial support of the Programma Giovani Ricercatori – Rita Levi Montalcini – Rientro dei Cervelli (2012) awarded by the Italian Ministry of Education, Universities and Research (MIUR). SaM would like to acknowledge support from the Ramon y Cajal fellowship number RYC-2015-17697. AJ, MH, and SA acknowledge support by the Danish Council for Independent Research, through a DFF Sapere Aude Starting Grant nr. 4181-00487B. SzCs, APH, MP, and HR acknowledge the support of the DFG priority program SPP 1992Exploring the Diversity of Extrasolar Planets (grants HA 3279/12-1, PA 525/18-1, PA5 25/19-1 and PA525/20-1, RA 714/14-1) HD, CR, and FPH acknowledge the financial support from MINECO under grants ESP2015-65712-C5-4-R and AYA2016-76378-P. This paper has made use of the IAC Supercomputing facility HTCondor (http://research.cs.wisc.edu/htcondor/), partly financed by the Ministry of Economy and Competitiveness with FEDER funds, code IACA13-3E-2493. MF and CMP gratefully acknowledge the support of the Swedish National Space Board. RAG and StM thanks the support of the CNES PLATO grant. PGB is a postdoctoral fellow in the MINECO-programme ’Juan de la Cierva Incorporacion’ (IJCI-2015-26034). StM acknowledges support from ERC through SPIRE grant (647383) and from ISSI through the ENCELADE 2.0 team. VSA acknowledges support from VILLUM FONDEN (research grant 10118). MNL acknowledges support from the ESA-PRODEX programme. Funding for the Stellar Astrophysics Centre is provided by The Danish National Research Foundation (Grant agreement no.: DNRF106) This work has made use of data from the European Space Agency (ESA) mission Gaia (https://www.cosmos.esa.int/gaia), processed by the Gaia Data Processing and Analysis Consortium (DPAC, https://www.cosmos.esa.int/web/gaia/dpac/consortium). Funding for the DPAC has been provided by national institutions, in particular the institutions participating in the Gaia Multilateral Agreement. This research was made with the use of NASA’s Astrophysics Data System and the NASA Exoplanet Archive, which is operated by the California Institute of Technology, under contract with the National Aeronautics and Space Administration under the Exoplanet Exploration Program.","date_updated":"2022-08-22T07:45:38Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_processing_charge":"No","issue":"4","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics","asteroseismology","planets and satellites: composition","planets and satellites: formation","planets and satellites: fundamental parameters"],"citation":{"ista":"Van Eylen V, Dai F, Mathur S, Gandolfi D, Albrecht S, Fridlund M, García RA, Guenther E, Hjorth M, Justesen AB, Livingston J, Lund MN, Pérez Hernández F, Prieto-Arranz J, Regulo C, Bugnet LA, Everett ME, Hirano T, Nespral D, Nowak G, Palle E, Silva Aguirre V, Trifonov T, Winn JN, Barragán O, Beck PG, Chaplin WJ, Cochran WD, Csizmadia S, Deeg H, Endl M, Heeren P, Grziwa S, Hatzes AP, Hidalgo D, Korth J, Mathis S, Montañes Rodriguez P, Narita N, Patzold M, Persson CM, Rodler F, Smith AMS. 2018. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 478(4), 4866–4880.","mla":"Van Eylen, V., et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 4, Oxford University Press, 2018, pp. 4866–80, doi:10.1093/mnras/sty1390.","chicago":"Van Eylen, V, F Dai, S Mathur, D Gandolfi, S Albrecht, M Fridlund, R A García, et al. “HD 89345: A Bright Oscillating Star Hosting a Transiting Warm Saturn-Sized Planet Observed by K2.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty1390.","short":"V. Van Eylen, F. Dai, S. Mathur, D. Gandolfi, S. Albrecht, M. Fridlund, R.A. García, E. Guenther, M. Hjorth, A.B. Justesen, J. Livingston, M.N. Lund, F. Pérez Hernández, J. Prieto-Arranz, C. Regulo, L.A. Bugnet, M.E. Everett, T. Hirano, D. Nespral, G. Nowak, E. Palle, V. Silva Aguirre, T. Trifonov, J.N. Winn, O. Barragán, P.G. Beck, W.J. Chaplin, W.D. Cochran, S. Csizmadia, H. Deeg, M. Endl, P. Heeren, S. Grziwa, A.P. Hatzes, D. Hidalgo, J. Korth, S. Mathis, P. Montañes Rodriguez, N. Narita, M. Patzold, C.M. Persson, F. Rodler, A.M.S. Smith, Monthly Notices of the Royal Astronomical Society 478 (2018) 4866–4880.","ieee":"V. Van Eylen et al., “HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2,” Monthly Notices of the Royal Astronomical Society, vol. 478, no. 4. Oxford University Press, pp. 4866–4880, 2018.","ama":"Van Eylen V, Dai F, Mathur S, et al. HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. 2018;478(4):4866-4880. doi:10.1093/mnras/sty1390","apa":"Van Eylen, V., Dai, F., Mathur, S., Gandolfi, D., Albrecht, S., Fridlund, M., … Smith, A. M. S. (2018). HD 89345: A bright oscillating star hosting a transiting warm Saturn-sized planet observed by K2. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty1390"},"page":"4866-4880","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1"},{"extern":"1","month":"03","external_id":{"arxiv":["1704.03516"]},"oa_version":"Published Version","day":"01","article_type":"original","publication_status":"published","abstract":[{"text":"Recent surveys of the Magellanic Clouds have revealed a subtype of Wolf–Rayet (WR) star with peculiar properties. WN3/O3 spectra exhibit both WR-like emission and O3 V-like absorption – but at lower luminosity than O3 V or WN stars. We examine the projected spatial distribution of WN3/O3 stars in the Large Magellanic Cloud as compared to O-type stars. Surprisingly, WN3/O3 stars are among the most isolated of all classes of massive stars; they have a distribution similar to red supergiants dominated by initial masses of 10–15 M⊙, and are far more dispersed than classical WR stars or luminous blue variables. Their lack of association with clusters of O-type stars suggests strongly that WN3/O3 stars are not the descendants of single massive stars (30 M⊙ or above). Instead, they are likely products of interacting binaries at lower initial mass (10–18 M⊙). Comparison with binary models suggests a probable origin with primaries in this mass range that were stripped of their H envelopes through non-conservative mass transfer by a low-mass secondary. We show that model spectra and positions on the Hertzsprung–Russell diagram for binary-stripped stars are consistent with WN3/O3 stars. Monitoring radial velocities with high-resolution spectra can test for low-mass companions or runaway velocities. With lower initial mass and environments that avoid very massive stars, the WN3/O3 stars fit expectations for progenitors of Type Ib and possibly Type Ibn supernovae.","lang":"eng"}],"arxiv":1,"year":"2018","oa":1,"volume":475,"date_published":"2018-03-01T00:00:00Z","_id":"13474","publisher":"Oxford University Press","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stx3181"}],"type":"journal_article","intvolume":" 475","date_created":"2023-08-03T10:14:47Z","author":[{"full_name":"Smith, Nathan","last_name":"Smith","first_name":"Nathan"},{"full_name":"Götberg, Ylva Louise Linsdotter","id":"d0648d0c-0f64-11ee-a2e0-dd0faa2e4f7d","orcid":"0000-0002-6960-6911","first_name":"Ylva Louise Linsdotter","last_name":"Götberg"},{"full_name":"de Mink, Selma E","first_name":"Selma E","last_name":"de Mink"}],"doi":"10.1093/mnras/stx3181","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"chicago":"Smith, Nathan, Ylva Louise Linsdotter Götberg, and Selma E de Mink. “Extreme Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the Elusive Stripped Binaries.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/stx3181.","ista":"Smith N, Götberg YLL, de Mink SE. 2018. Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. Monthly Notices of the Royal Astronomical Society. 475(1), 772–782.","mla":"Smith, Nathan, et al. “Extreme Isolation of WN3/O3 Stars and Implications for Their Evolutionary Origin as the Elusive Stripped Binaries.” Monthly Notices of the Royal Astronomical Society, vol. 475, no. 1, Oxford University Press, 2018, pp. 772–82, doi:10.1093/mnras/stx3181.","short":"N. Smith, Y.L.L. Götberg, S.E. de Mink, Monthly Notices of the Royal Astronomical Society 475 (2018) 772–782.","ama":"Smith N, Götberg YLL, de Mink SE. Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. Monthly Notices of the Royal Astronomical Society. 2018;475(1):772-782. doi:10.1093/mnras/stx3181","apa":"Smith, N., Götberg, Y. L. L., & de Mink, S. E. (2018). Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stx3181","ieee":"N. Smith, Y. L. L. Götberg, and S. E. de Mink, “Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries,” Monthly Notices of the Royal Astronomical Society, vol. 475, no. 1. Oxford University Press, pp. 772–782, 2018."},"page":"772-782","scopus_import":"1","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"status":"public","language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","article_processing_charge":"No","title":"Extreme isolation of WN3/O3 stars and implications for their evolutionary origin as the elusive stripped binaries","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"date_updated":"2023-08-09T12:17:34Z"},{"oa_version":"Preprint","external_id":{"arxiv":["1802.08248"]},"day":"23","extern":"1","month":"02","arxiv":1,"volume":476,"date_published":"2018-02-23T00:00:00Z","oa":1,"year":"2018","abstract":[{"lang":"eng","text":"Radio pulsars found in binary systems with short orbital periods are usually fast spinning as a consequence of recycling via mass transfer from their companion stars; this process is also thought to decrease the magnetic field of the neutron star being recycled. Here, we report on timing observations of the recently discovered binary PSR J1755−2550 and find that this pulsar is an exception: with a characteristic age of 2.1 Myr, it is relatively young; furthermore, with a spin period of 315 ms and a surface magnetic field strength at its poles of 0.88 × 1012 G, the pulsar shows no sign of having been recycled. Based on its timing and orbital characteristics, the pulsar either has a massive white dwarf (WD) or a neutron star (NS) companion. To distinguish between these two cases, we searched radio observations for a potential recycled pulsar companion and analysed archival optical data for a potential WD companion. Neither work returned conclusive detections. We apply population synthesis modelling and find that both solutions are roughly equally probable. Our population synthesis also predicts a minimum mass of 0.90 M⊙ for the companion star to PSR J1755−2550 and we simulate the systemic runaway velocities for the resulting WDNS systems which may merge and possibly produce Ca-rich supernovae. Whether PSR J1755−2550 hosts a WD or a NS companion star, it is certainly a member of a rare subpopulation of binary radio pulsars."}],"article_type":"original","publication_status":"published","_id":"15236","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.1802.08248","open_access":"1"}],"publisher":"Oxford University Press","author":[{"last_name":"Ng","first_name":"C","full_name":"Ng, C"},{"first_name":"M U","last_name":"Kruckow","full_name":"Kruckow, M U"},{"full_name":"Tauris, T M","last_name":"Tauris","first_name":"T M"},{"full_name":"Lyne, A G","first_name":"A G","last_name":"Lyne"},{"full_name":"Freire, P C C","first_name":"P C C","last_name":"Freire"},{"full_name":"Ridolfi, A","first_name":"A","last_name":"Ridolfi"},{"first_name":"Ilaria","last_name":"Caiazzo","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388"},{"last_name":"Heyl","first_name":"J","full_name":"Heyl, J"},{"full_name":"Kramer, M","last_name":"Kramer","first_name":"M"},{"full_name":"Cameron, A D","first_name":"A D","last_name":"Cameron"},{"full_name":"Champion, D J","first_name":"D J","last_name":"Champion"},{"full_name":"Stappers, B","last_name":"Stappers","first_name":"B"}],"date_created":"2024-03-26T10:39:05Z","doi":"10.1093/mnras/sty482","intvolume":" 476","type":"journal_article","issue":"4","status":"public","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"citation":{"chicago":"Ng, C, M U Kruckow, T M Tauris, A G Lyne, P C C Freire, A Ridolfi, Ilaria Caiazzo, et al. “PSR J1755−2550: A Young Radio Pulsar with a Massive, Compact Companion.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty482.","ista":"Ng C, Kruckow MU, Tauris TM, Lyne AG, Freire PCC, Ridolfi A, Caiazzo I, Heyl J, Kramer M, Cameron AD, Champion DJ, Stappers B. 2018. PSR J1755−2550: A young radio pulsar with a massive, compact companion. Monthly Notices of the Royal Astronomical Society. 476(4), 4315–4326.","mla":"Ng, C., et al. “PSR J1755−2550: A Young Radio Pulsar with a Massive, Compact Companion.” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4, Oxford University Press, 2018, pp. 4315–26, doi:10.1093/mnras/sty482.","short":"C. Ng, M.U. Kruckow, T.M. Tauris, A.G. Lyne, P.C.C. Freire, A. Ridolfi, I. Caiazzo, J. Heyl, M. Kramer, A.D. Cameron, D.J. Champion, B. Stappers, Monthly Notices of the Royal Astronomical Society 476 (2018) 4315–4326.","ama":"Ng C, Kruckow MU, Tauris TM, et al. PSR J1755−2550: A young radio pulsar with a massive, compact companion. Monthly Notices of the Royal Astronomical Society. 2018;476(4):4315-4326. doi:10.1093/mnras/sty482","apa":"Ng, C., Kruckow, M. U., Tauris, T. M., Lyne, A. G., Freire, P. C. C., Ridolfi, A., … Stappers, B. (2018). PSR J1755−2550: A young radio pulsar with a massive, compact companion. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty482","ieee":"C. Ng et al., “PSR J1755−2550: A young radio pulsar with a massive, compact companion,” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 4. Oxford University Press, pp. 4315–4326, 2018."},"page":"4315-4326","publication":"Monthly Notices of the Royal Astronomical Society","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"quality_controlled":"1","title":"PSR J1755−2550: A young radio pulsar with a massive, compact companion","date_updated":"2024-04-08T07:02:52Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"article_processing_charge":"No"},{"issue":"4","scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"4383-4396","citation":{"chicago":"Fontecilla, Camilo, Zoltán Haiman, and Jorge Cuadra. “Non-Steady-State Long-Term Evolution of Supermassive Black Hole Binaries Surrounded by Accretion Discs.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty2972.","mla":"Fontecilla, Camilo, et al. “Non-Steady-State Long-Term Evolution of Supermassive Black Hole Binaries Surrounded by Accretion Discs.” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 4, Oxford University Press, 2018, pp. 4383–96, doi:10.1093/mnras/sty2972.","ista":"Fontecilla C, Haiman Z, Cuadra J. 2018. Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs. Monthly Notices of the Royal Astronomical Society. 482(4), 4383–4396.","short":"C. Fontecilla, Z. Haiman, J. Cuadra, Monthly Notices of the Royal Astronomical Society 482 (2018) 4383–4396.","ama":"Fontecilla C, Haiman Z, Cuadra J. Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs. Monthly Notices of the Royal Astronomical Society. 2018;482(4):4383-4396. doi:10.1093/mnras/sty2972","apa":"Fontecilla, C., Haiman, Z., & Cuadra, J. (2018). Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty2972","ieee":"C. Fontecilla, Z. Haiman, and J. Cuadra, “Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs,” Monthly Notices of the Royal Astronomical Society, vol. 482, no. 4. Oxford University Press, pp. 4383–4396, 2018."},"status":"public","quality_controlled":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"article_processing_charge":"No","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_updated":"2024-09-18T09:58:03Z","title":"Non-steady-state long-term evolution of supermassive black hole binaries surrounded by accretion discs","month":"11","extern":"1","day":"06","oa_version":"Published Version","publication_status":"published","article_type":"original","abstract":[{"text":"Supermassive black holes (SMBHs) pair and form bound binaries after their host galaxies merge. In a gas-rich merger, accretion discs are expected to form around the binary and its components. These discs control the binary orbital evolution until the system is compact enough for gravitational waves to drive the SMBHs to coalescence. In this work, we implemented a time-dependent one-dimensional model to follow the long-term evolution of the coupled binary+disc system, from a separation of 10^5 down to 20 Schwarzschild radii. We run different models changing the system parameters, including the binary mass ratio q ≤ 0.3 and a factor of γ that controls the inflow across the gap created by the secondary. We find that our implementation yields higher residual masses and longer binary residence times than previous studies. Our main conclusion is the non-steady-state nature of the evolution of the system: the properties the disc had when the binary was still at large separations influence its whole evolution. To recover steady state, the binary residence time would have to be much longer than the inflow time-scale of the disc throughout their entire history, which in general is not satisfied.","lang":"eng"}],"year":"2018","oa":1,"volume":482,"date_published":"2018-11-06T00:00:00Z","publisher":"Oxford University Press","main_file_link":[{"url":"https://doi.org/10.1093/mnras/sty2972","open_access":"1"}],"_id":"17550","intvolume":" 482","type":"journal_article","doi":"10.1093/mnras/sty2972","date_created":"2024-09-05T10:12:03Z","author":[{"full_name":"Fontecilla, Camilo","last_name":"Fontecilla","first_name":"Camilo"},{"last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán"},{"first_name":"Jorge","last_name":"Cuadra","full_name":"Cuadra, Jorge"}]},{"scopus_import":"1","publication":"Monthly Notices of the Royal Astronomical Society","page":"2249-2257","citation":{"ieee":"Y. Tang, Z. Haiman, and A. MacFadyen, “The late inspiral of supermassive black hole binaries with circumbinary gas discs in the LISA band,” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 2. Oxford University Press, pp. 2249–2257, 2018.","ama":"Tang Y, Haiman Z, MacFadyen A. The late inspiral of supermassive black hole binaries with circumbinary gas discs in the LISA band. Monthly Notices of the Royal Astronomical Society. 2018;476(2):2249-2257. doi:10.1093/mnras/sty423","apa":"Tang, Y., Haiman, Z., & MacFadyen, A. (2018). The late inspiral of supermassive black hole binaries with circumbinary gas discs in the LISA band. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/sty423","ista":"Tang Y, Haiman Z, MacFadyen A. 2018. The late inspiral of supermassive black hole binaries with circumbinary gas discs in the LISA band. Monthly Notices of the Royal Astronomical Society. 476(2), 2249–2257.","mla":"Tang, Yike, et al. “The Late Inspiral of Supermassive Black Hole Binaries with Circumbinary Gas Discs in the LISA Band.” Monthly Notices of the Royal Astronomical Society, vol. 476, no. 2, Oxford University Press, 2018, pp. 2249–57, doi:10.1093/mnras/sty423.","chicago":"Tang, Yike, Zoltán Haiman, and Andrew MacFadyen. “The Late Inspiral of Supermassive Black Hole Binaries with Circumbinary Gas Discs in the LISA Band.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2018. https://doi.org/10.1093/mnras/sty423.","short":"Y. Tang, Z. Haiman, A. MacFadyen, Monthly Notices of the Royal Astronomical Society 476 (2018) 2249–2257."},"status":"public","issue":"2","article_processing_charge":"No","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_updated":"2024-09-24T08:18:22Z","title":"The late inspiral of supermassive black hole binaries with circumbinary gas discs in the LISA band","quality_controlled":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","language":[{"iso":"eng"}],"publication_status":"published","article_type":"original","abstract":[{"text":"We present the results of 2D, moving-mesh, viscous hydrodynamical simulations of an accretion disc around a merging supermassive black hole binary (SMBHB). The simulation is pseudo-Newtonian, with the BHs modelled as point masses with a Paczynski–Wiita potential, and includes viscous heating, shock heating, and radiative cooling. We follow the gravitational inspiral of an equal-mass binary with a component mass Mbh = 106 M⊙ from an initial separation of 60rg (where rg ≡ GMbh/c2 is the gravitational radius) to the merger. We find that a central, low-density cavity forms around the binary, as in previous work, but that the BHs capture gas from the circumbinary disc and accrete efficiently via their own minidiscs, well after their inspiral outpaces the viscous evolution of the disc. The system remains luminous, displaying strong periodicity at twice the binary orbital frequency throughout the entire inspiral process, all the way to the merger. In the soft X-ray band, the thermal emission is dominated by the inner edge of the circumbinary disc with especially clear periodicity in the early inspiral. By comparison, harder X-ray emission is dominated by the minidiscs, and the light curve is initially more noisy but develops a clear periodicity in the late inspiral stage. This variability pattern should help identify the electromagnetic counterparts of SMBHBs detected by the space-based gravitational-wave detector LISA.","lang":"eng"}],"oa":1,"year":"2018","volume":476,"date_published":"2018-02-19T00:00:00Z","month":"02","extern":"1","day":"19","oa_version":"Published Version","intvolume":" 476","type":"journal_article","doi":"10.1093/mnras/sty423","author":[{"first_name":"Yike","last_name":"Tang","full_name":"Tang, Yike"},{"full_name":"Haiman, Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","last_name":"Haiman"},{"full_name":"MacFadyen, Andrew","last_name":"MacFadyen","first_name":"Andrew"}],"date_created":"2024-09-05T13:47:09Z","main_file_link":[{"url":"https://doi.org/10.1093/mnras/sty423","open_access":"1"}],"publisher":"Oxford University Press","_id":"17619"}]