[{"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17655","publication_identifier":{"issn":["0035-8711","1365-2966"]},"citation":{"chicago":"Visbal, Eli, Zoltán Haiman, and Greg L Bryan. “Self-Consistent Semi-Analytic Models of the First Stars.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty142\">https://doi.org/10.1093/mnras/sty142</a>.","ieee":"E. Visbal, Z. Haiman, and G. L. Bryan, “Self-consistent semi-analytic models of the first stars,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 4. Oxford University Press, pp. 5246–5256, 2018.","mla":"Visbal, Eli, et al. “Self-Consistent Semi-Analytic Models of the First Stars.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 475, no. 4, Oxford University Press, 2018, pp. 5246–56, doi:<a href=\"https://doi.org/10.1093/mnras/sty142\">10.1093/mnras/sty142</a>.","ista":"Visbal E, Haiman Z, Bryan GL. 2018. Self-consistent semi-analytic models of the first stars. Monthly Notices of the Royal Astronomical Society. 475(4), 5246–5256.","short":"E. Visbal, Z. Haiman, G.L. Bryan, Monthly Notices of the Royal Astronomical Society 475 (2018) 5246–5256.","apa":"Visbal, E., Haiman, Z., &#38; Bryan, G. L. (2018). Self-consistent semi-analytic models of the first stars. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty142\">https://doi.org/10.1093/mnras/sty142</a>","ama":"Visbal E, Haiman Z, Bryan GL. Self-consistent semi-analytic models of the first stars. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;475(4):5246-5256. doi:<a href=\"https://doi.org/10.1093/mnras/sty142\">10.1093/mnras/sty142</a>"},"title":"Self-consistent semi-analytic models of the first stars","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/sty142"}],"date_created":"2024-09-06T07:33:13Z","extern":"1","month":"01","scopus_import":"1","oa":1,"article_type":"original","publication_status":"published","year":"2018","intvolume":"       475","date_updated":"2024-09-24T14:23:23Z","day":"17","publisher":"Oxford University Press","author":[{"last_name":"Visbal","full_name":"Visbal, Eli","first_name":"Eli"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"first_name":"Greg L","last_name":"Bryan","full_name":"Bryan, Greg L"}],"type":"journal_article","oa_version":"Published Version","issue":"4","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"We have developed a semi-analytic framework to model the large-scale evolution of the first Population III (Pop III) stars and the transition to metal-enriched star formation. Our model follows dark matter haloes from cosmological N-body simulations, utilizing their individual merger histories and three-dimensional positions, and applies physically motivated prescriptions for star formation and feedback from Lyman–Werner (LW) radiation, hydrogen ionizing radiation, and external metal enrichment due to supernovae winds. This method is intended to complement analytic studies, which do not include clustering or individual merger histories, and hydrodynamical cosmological simulations, which include detailed physics, but are computationally expensive and have limited dynamic range. Utilizing this technique, we compute the cumulative Pop III and metal-enriched star formation rate density (SFRD) as a function of redshift at z ≥ 20. We find that varying the model parameters leads to significant qualitative changes in the global star formation history. The Pop III star formation efficiency and the delay time between Pop III and subsequent metal-enriched star formation are found to have the largest impact. The effect of clustering (i.e. including the three-dimensional positions of individual haloes) on various feedback mechanisms is also investigated. The impact of clustering on LW and ionization feedback is found to be relatively mild in our fiducial model, but can be larger if external metal enrichment can promote metal-enriched star formation over large distances.","lang":"eng"}],"status":"public","date_published":"2018-01-17T00:00:00Z","language":[{"iso":"eng"}],"volume":475,"page":"5246-5256","article_processing_charge":"No","doi":"10.1093/mnras/sty142"},{"year":"2018","intvolume":"       476","month":"02","oa":1,"scopus_import":"1","article_type":"original","publication_status":"published","citation":{"mla":"Inayoshi, Kohei, et al. “Low-Density, Radiatively Inefficient Rotating-Accretion Flow on to a Black Hole.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 1, Oxford University Press, 2018, pp. 1412–26, doi:<a href=\"https://doi.org/10.1093/mnras/sty276\">10.1093/mnras/sty276</a>.","chicago":"Inayoshi, Kohei, Jeremiah P Ostriker, Zoltán Haiman, and Rolf Kuiper. “Low-Density, Radiatively Inefficient Rotating-Accretion Flow on to a Black Hole.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty276\">https://doi.org/10.1093/mnras/sty276</a>.","ieee":"K. Inayoshi, J. P. Ostriker, Z. Haiman, and R. Kuiper, “Low-density, radiatively inefficient rotating-accretion flow on to a black hole,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 1. Oxford University Press, pp. 1412–1426, 2018.","ama":"Inayoshi K, Ostriker JP, Haiman Z, Kuiper R. Low-density, radiatively inefficient rotating-accretion flow on to a black hole. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(1):1412-1426. doi:<a href=\"https://doi.org/10.1093/mnras/sty276\">10.1093/mnras/sty276</a>","apa":"Inayoshi, K., Ostriker, J. P., Haiman, Z., &#38; Kuiper, R. (2018). Low-density, radiatively inefficient rotating-accretion flow on to a black hole. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty276\">https://doi.org/10.1093/mnras/sty276</a>","ista":"Inayoshi K, Ostriker JP, Haiman Z, Kuiper R. 2018. Low-density, radiatively inefficient rotating-accretion flow on to a black hole. Monthly Notices of the Royal Astronomical Society. 476(1), 1412–1426.","short":"K. Inayoshi, J.P. Ostriker, Z. Haiman, R. Kuiper, Monthly Notices of the Royal Astronomical Society 476 (2018) 1412–1426."},"title":"Low-density, radiatively inefficient rotating-accretion flow on to a black hole","quality_controlled":"1","date_created":"2024-09-06T08:05:18Z","main_file_link":[{"url":"https://doi.org/10.1093/mnras/sty276","open_access":"1"}],"extern":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17679","publication_identifier":{"issn":["0035-8711","1365-2966"]},"language":[{"iso":"eng"}],"date_published":"2018-02-01T00:00:00Z","volume":476,"page":"1412-1426","doi":"10.1093/mnras/sty276","article_processing_charge":"No","oa_version":"Published Version","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"We study low-density axisymmetric accretion flows onto black holes (BHs) with two-dimensional hydrodynamical simulations, adopting the α-viscosity prescription. When the gas angular momentum is low enough to form a rotationally supported disk within the Bondi radius (RB), we find a global steady accretion solution. The solution consists of a rotational equilibrium distribution at r∼RB, where the density follows ρ∝(1+RB/r)^3/2, surrounding a geometrically thick and optically thin accretion disk at the centrifugal radius, where thermal energy generated by viscosity is transported via strong convection. Physical properties of the inner solution agree with those expected in convection-dominated accretion flows (CDAF; ρ∝r^−1/2). In the inner CDAF solution, the gas inflow rate decreases towards the center due to convection (M˙∝r), and the net accretion rate (including both inflows and outflows) is strongly suppressed by several orders of magnitude from the Bondi accretion rate M˙B The net accretion rate depends on the viscous strength, following M˙/M˙B∝(α/0.01)^0.6. This solution holds for low accretion rates of M˙B/M˙Edd<10^−3 having minimal radiation cooling, where M˙Edd is the Eddington rate. In a hot plasma at the bottom (r<10^−3 RB), thermal conduction would dominate the convective energy flux. Since suppression of the accretion by convection ceases, the final BH feeding rate is found to be M˙/M˙B∼10^−3−10^−2. This rate is as low as M˙/M˙Edd∼10^−7−10^−6 inferred for SgrA∗ and the nuclear BHs in M31 and M87, and can explain the low luminosities in these sources, without invoking any feedback mechanism.","lang":"eng"}],"status":"public","publisher":"Oxford University Press","author":[{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"last_name":"Ostriker","full_name":"Ostriker, Jeremiah P","first_name":"Jeremiah P"},{"last_name":"Haiman","full_name":"Haiman, Zoltán","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"last_name":"Kuiper","full_name":"Kuiper, Rolf","first_name":"Rolf"}],"type":"journal_article","date_updated":"2024-09-25T08:57:35Z","day":"01"},{"publisher":"Oxford University Press","author":[{"last_name":"Inayoshi","full_name":"Inayoshi, Kohei","first_name":"Kohei"},{"first_name":"Miao","last_name":"Li","full_name":"Li, Miao"},{"full_name":"Haiman, Zoltán","last_name":"Haiman","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán"}],"type":"journal_article","date_updated":"2024-09-25T09:46:30Z","day":"30","language":[{"iso":"eng"}],"date_published":"2018-06-30T00:00:00Z","volume":479,"page":"4017-4027","doi":"10.1093/mnras/sty1720","article_processing_charge":"No","oa_version":"Published Version","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"lang":"eng","text":"We propose the formation of massive pristine dark-matter (DM) halos with masses of ∼10^8 M⊙, due to the dynamical effects of frequent mergers in rare regions of the Universe with high baryonic streaming velocity relative to DM. Since the streaming motion prevents gas collapse into DM halos and delays prior star formation episodes, the gas remains metal-free until the halo virial temperatures ≳2×10^4 K. The minimum cooling mass of DM halos is boosted by a factor of ∼10−30 because frequent major mergers of halos further inhibit gas collapse. We use Monte Carlo merger trees to simulate the DM assembly history under a streaming velocity of twice the root-mean-square value, and estimate the number density of massive DM halos containing pristine gas as ≃10^−4 cMpc^−3. When the gas infall begins, efficient Lyα cooling drives cold streams penetrating inside the halo and feeding a central galactic disk. When one stream collides with the disk, strong shock forms a dense and hot gas cloud, where the gas never forms H2 molecules due to effective collisional dissociation. As a result, a massive gas cloud forms by gravitational instability and collapses directly into a massive black hole (BH) with M∙∼10^5 M⊙. Almost simultaneously, a galaxy with M⋆,tot∼10^6 M⊙ composed of Population III stars forms in the nuclear region. If the typical stellar mass is as high as ∼100 M⊙, the galaxy could be detected with the James Webb Space Telescope even at z≳15. These massive seed BHs would be fed by continuous gas accretion from the host galaxy, and grow to be bright quasars observed at z≳6."}],"status":"public","citation":{"apa":"Inayoshi, K., Li, M., &#38; Haiman, Z. (2018). Massive black hole and Population III galaxy formation in overmassive dark-matter haloes with violent merger histories. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty1720\">https://doi.org/10.1093/mnras/sty1720</a>","ama":"Inayoshi K, Li M, Haiman Z. Massive black hole and Population III galaxy formation in overmassive dark-matter haloes with violent merger histories. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;479(3):4017-4027. doi:<a href=\"https://doi.org/10.1093/mnras/sty1720\">10.1093/mnras/sty1720</a>","short":"K. Inayoshi, M. Li, Z. Haiman, Monthly Notices of the Royal Astronomical Society 479 (2018) 4017–4027.","ista":"Inayoshi K, Li M, Haiman Z. 2018. Massive black hole and Population III galaxy formation in overmassive dark-matter haloes with violent merger histories. Monthly Notices of the Royal Astronomical Society. 479(3), 4017–4027.","mla":"Inayoshi, Kohei, et al. “Massive Black Hole and Population III Galaxy Formation in Overmassive Dark-Matter Haloes with Violent Merger Histories.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 479, no. 3, Oxford University Press, 2018, pp. 4017–27, doi:<a href=\"https://doi.org/10.1093/mnras/sty1720\">10.1093/mnras/sty1720</a>.","ieee":"K. Inayoshi, M. Li, and Z. Haiman, “Massive black hole and Population III galaxy formation in overmassive dark-matter haloes with violent merger histories,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 479, no. 3. Oxford University Press, pp. 4017–4027, 2018.","chicago":"Inayoshi, Kohei, Miao Li, and Zoltán Haiman. “Massive Black Hole and Population III Galaxy Formation in Overmassive Dark-Matter Haloes with Violent Merger Histories.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty1720\">https://doi.org/10.1093/mnras/sty1720</a>."},"title":"Massive black hole and Population III galaxy formation in overmassive dark-matter haloes with violent merger histories","quality_controlled":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/sty1720"}],"date_created":"2024-09-06T08:22:23Z","extern":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17687","publication_identifier":{"issn":["0035-8711","1365-2966"]},"year":"2018","intvolume":"       479","month":"06","oa":1,"article_type":"original","scopus_import":"1","publication_status":"published"},{"year":"2018","intvolume":"       476","month":"02","article_type":"original","scopus_import":"1","oa":1,"publication_status":"published","citation":{"short":"M. Charisi, Z. Haiman, D. Schiminovich, D.J. D’Orazio, Monthly Notices of the Royal Astronomical Society 476 (2018) 4617–4628.","ista":"Charisi M, Haiman Z, Schiminovich D, D’Orazio DJ. 2018. Testing the relativistic Doppler boost hypothesis for supermassive black hole binary candidates. Monthly Notices of the Royal Astronomical Society. 476(4), 4617–4628.","ama":"Charisi M, Haiman Z, Schiminovich D, D’Orazio DJ. Testing the relativistic Doppler boost hypothesis for supermassive black hole binary candidates. <i>Monthly Notices of the Royal Astronomical Society</i>. 2018;476(4):4617-4628. doi:<a href=\"https://doi.org/10.1093/mnras/sty516\">10.1093/mnras/sty516</a>","apa":"Charisi, M., Haiman, Z., Schiminovich, D., &#38; D’Orazio, D. J. (2018). Testing the relativistic Doppler boost hypothesis for supermassive black hole binary candidates. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/sty516\">https://doi.org/10.1093/mnras/sty516</a>","ieee":"M. Charisi, Z. Haiman, D. Schiminovich, and D. J. D’Orazio, “Testing the relativistic Doppler boost hypothesis for supermassive black hole binary candidates,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4. Oxford University Press, pp. 4617–4628, 2018.","chicago":"Charisi, Maria, Zoltán Haiman, David Schiminovich, and Daniel J D’Orazio. “Testing the Relativistic Doppler Boost Hypothesis for Supermassive Black Hole Binary Candidates.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2018. <a href=\"https://doi.org/10.1093/mnras/sty516\">https://doi.org/10.1093/mnras/sty516</a>.","mla":"Charisi, Maria, et al. “Testing the Relativistic Doppler Boost Hypothesis for Supermassive Black Hole Binary Candidates.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 476, no. 4, Oxford University Press, 2018, pp. 4617–28, doi:<a href=\"https://doi.org/10.1093/mnras/sty516\">10.1093/mnras/sty516</a>."},"title":"Testing the relativistic Doppler boost hypothesis for supermassive black hole binary candidates","quality_controlled":"1","main_file_link":[{"url":"https://doi.org/10.1093/mnras/sty516","open_access":"1"}],"date_created":"2024-09-06T08:38:11Z","extern":"1","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17691","publication_identifier":{"issn":["0035-8711","1365-2966"]},"date_published":"2018-02-28T00:00:00Z","language":[{"iso":"eng"}],"volume":476,"page":"4617-4628","doi":"10.1093/mnras/sty516","article_processing_charge":"No","oa_version":"Published Version","issue":"4","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"lang":"eng","text":"Supermassive black hole binaries (SMBHBs) should be common in galactic nuclei as a result of frequent galaxy mergers. Recently, a large sample of sub-parsec SMBHB candidates was identified as bright periodically variable quasars in optical surveys. If the observed periodicity corresponds to the redshifted binary orbital period, the inferred orbital velocities are relativistic (v/c ≈ 0.1). The optical and ultraviolet (UV) luminosities are expected to arise from gas bound to the individual BHs, and would be modulated by the relativistic Doppler effect. The optical and UV light curves should vary in tandem with relative amplitudes which depend on the respective spectral slopes. We constructed a control sample of 42 quasars with aperiodic variability, to test whether this Doppler colour signature can be distinguished from intrinsic chromatic variability. We found that the Doppler signature can arise by chance in ∼20 per cent (∼37 per cent) of quasars in the nUV (fUV) band. These probabilities reflect the limited quality of the control sample and represent upper limits on how frequently quasars mimic the Doppler brightness+colour variations. We performed separate tests on the periodic quasar candidates, and found that for the majority, the Doppler boost hypothesis requires an unusually steep UV spectrum or an unexpectedly large BH mass and orbital velocity. We conclude that at most approximately one-third of these periodic candidates can harbor Doppler-modulated SMBHBs."}],"status":"public","publisher":"Oxford University Press","author":[{"first_name":"Maria","full_name":"Charisi, Maria","last_name":"Charisi"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"first_name":"David","last_name":"Schiminovich","full_name":"Schiminovich, David"},{"first_name":"Daniel J","full_name":"D'Orazio, Daniel J","last_name":"D'Orazio"}],"type":"journal_article","date_updated":"2024-09-25T09:56:16Z","day":"28"},{"type":"journal_article","publisher":"Oxford University Press","author":[{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","last_name":"Matthee"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Philip","last_name":"Best","full_name":"Best, Philip"},{"last_name":"Smail","full_name":"Smail, Ian","first_name":"Ian"},{"first_name":"Fuyan","last_name":"Bian","full_name":"Bian, Fuyan"},{"full_name":"Darvish, Behnam","last_name":"Darvish","first_name":"Behnam"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"first_name":"Xiaohui","full_name":"Fan, Xiaohui","last_name":"Fan"}],"day":"01","date_updated":"2024-10-14T11:34:07Z","volume":471,"doi":"10.1093/mnras/stx1569","article_processing_charge":"No","page":"629-649","date_published":"2017-10-01T00:00:00Z","language":[{"iso":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","status":"public","abstract":[{"text":"We present a sample of ∼1000 emission-line galaxies at z = 0.4–4.7 from the ∼0.7deg2 High-z Emission-Line Survey in the Boötes field identified with a suite of six narrow-band filters at ≈0.4–2.1 μm. These galaxies have been selected on their Ly α (73), [O II] (285), H β/[O III] (387) or H α (362) emission line, and have been classified with optical to near-infrared colours. A subsample of 98 sources have reliable redshifts from multiple narrow-band (e.g. [O II]–H α) detections and/or spectroscopy. In this survey paper, we present the observations, selection and catalogues of emitters. We measure number densities of Ly α, [O II], H β/[O III] and H α and confirm strong luminosity evolution in star-forming galaxies from z ∼ 0.4 to ∼5, in agreement with previous results. To demonstrate the usefulness of dual-line emitters, we use the sample of dual [O II]–H α emitters to measure the observed [O II]/H α ratio at z = 1.47. The observed [O II]/H α ratio increases significantly from 0.40 ± 0.01 at z = 0.1 to 0.52 ± 0.05 at z = 1.47, which we attribute to either decreasing dust attenuation with redshift, or due to a bias in the (typically) fibre measurements in the local Universe that only measure the central kpc regions. At the bright end, we find that both the H α and Ly α number densities at z ≈ 2.2 deviate significantly from a Schechter form, following a power law. We show that this is driven entirely by an increasing X-ray/active galactic nucleus fraction with line luminosity, which reaches ≈100 per cent at line luminosities L ≳ 3 × 1044 erg s−1.","lang":"eng"}],"oa_version":"Preprint","quality_controlled":"1","title":"Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7","extern":"1","date_created":"2022-07-12T11:01:35Z","main_file_link":[{"url":"https://arxiv.org/abs/1702.04721","open_access":"1"}],"citation":{"apa":"Matthee, J. J., Sobral, D., Best, P., Smail, I., Bian, F., Darvish, B., … Fan, X. (2017). Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>","ama":"Matthee JJ, Sobral D, Best P, et al. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(1):629-649. doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>","ista":"Matthee JJ, Sobral D, Best P, Smail I, Bian F, Darvish B, Röttgering H, Fan X. 2017. Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7. Monthly Notices of the Royal Astronomical Society. 471(1), 629–649.","short":"J.J. Matthee, D. Sobral, P. Best, I. Smail, F. Bian, B. Darvish, H. Röttgering, X. Fan, Monthly Notices of the Royal Astronomical Society 471 (2017) 629–649.","mla":"Matthee, Jorryt J., et al. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1, Oxford University Press, 2017, pp. 629–49, doi:<a href=\"https://doi.org/10.1093/mnras/stx1569\">10.1093/mnras/stx1569</a>.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ian Smail, Fuyan Bian, Behnam Darvish, Huub Röttgering, and Xiaohui Fan. “Boötes-HiZELS: An Optical to near-Infrared Survey of Emission-Line Galaxies at z = 0.4–4.7.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1569\">https://doi.org/10.1093/mnras/stx1569</a>.","ieee":"J. J. Matthee <i>et al.</i>, “Boötes-HiZELS: An optical to near-infrared survey of emission-line galaxies at z = 0.4–4.7,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 1. Oxford University Press, pp. 629–649, 2017."},"publication_identifier":{"issn":["0035-8711","1365-2966"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11561","keyword":["Space and Planetary Science","Astronomy and Astrophysics galaxies","active","galaxies","evolution","galaxies","high-redshift","galaxies","luminosity function","mass function","galaxies: star formation"],"intvolume":"       471","year":"2017","arxiv":1,"external_id":{"arxiv":["1702.04721"]},"scopus_import":"1","oa":1,"article_type":"original","publication_status":"published","month":"10"},{"citation":{"mla":"Sobral, David, et al. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1, Oxford University Press, 2017, pp. 1242–58, doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>.","ieee":"D. Sobral <i>et al.</i>, “The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 466, no. 1. Oxford University Press, pp. 1242–1258, 2017.","chicago":"Sobral, David, Jorryt J Matthee, Philip Best, Andra Stroe, Huub Röttgering, Iván Oteo, Ian Smail, Leah Morabito, and Ana Paulino-Afonso. “The CALYMHA Survey: Lyα Luminosity Function and Global Escape Fraction of Lyα Photons at z = 2.23.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>.","apa":"Sobral, D., Matthee, J. J., Best, P., Stroe, A., Röttgering, H., Oteo, I., … Paulino-Afonso, A. (2017). The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw3090\">https://doi.org/10.1093/mnras/stw3090</a>","ama":"Sobral D, Matthee JJ, Best P, et al. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;466(1):1242-1258. doi:<a href=\"https://doi.org/10.1093/mnras/stw3090\">10.1093/mnras/stw3090</a>","short":"D. Sobral, J.J. Matthee, P. Best, A. Stroe, H. Röttgering, I. Oteo, I. Smail, L. Morabito, A. Paulino-Afonso, Monthly Notices of the Royal Astronomical Society 466 (2017) 1242–1258.","ista":"Sobral D, Matthee JJ, Best P, Stroe A, Röttgering H, Oteo I, Smail I, Morabito L, Paulino-Afonso A. 2017. The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23. Monthly Notices of the Royal Astronomical Society. 466(1), 1242–1258."},"title":"The CALYMHA survey: Lyα luminosity function and global escape fraction of Lyα photons at z = 2.23","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1609.05897","open_access":"1"}],"date_created":"2022-07-12T12:04:16Z","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11562","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"arxiv":1,"external_id":{"arxiv":["1609.05897"]},"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: haloes","galaxies: high-redshift","galaxies: luminosity function","mass function","galaxies: statistics","cosmology: observations"],"intvolume":"       466","month":"04","oa":1,"article_type":"original","scopus_import":"1","acknowledgement":"We thank the reviewer for his/her helpful comments and suggestions that have greatly improved this work. DS and JM acknowledge financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship. DS also acknowledges funding from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IRS acknowledges support from STFC (ST/L00075X/1), the ERC Advanced Investigator programme DUSTYGAL 321334 and a Royal Society/Wolfson merit award. We thank Matthew Hayes, Ryan Trainor, Kimihiko Nakajima and Anne Verhamme for many helpful discussions and Ana Sobral, Carolina Duarte and Miguel Domingos for taking part in observations with the NB392 filter. We also thank Sergio Santos for helpful comments. This research is based on observations obtained on the Isaac Newton Telescope (INT), programs: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B & I15AN008. The authors acknowledge the award of time from programmes: I13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008 on the INT. 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. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme ID 098.A 0819. We have benefited greatly from the publicly available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP (Bertin & Arnouts 1996; Bertin 2010), SCAMP (Bertin 2006) and TOPCAT (Taylor 2005). Dedicated to the memory of M. L. Nicolau and M. C. Serrano.","publication_status":"published","publisher":"Oxford University Press","author":[{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Best","full_name":"Best, Philip","first_name":"Philip"},{"last_name":"Stroe","full_name":"Stroe, Andra","first_name":"Andra"},{"full_name":"Röttgering, Huub","last_name":"Röttgering","first_name":"Huub"},{"first_name":"Iván","last_name":"Oteo","full_name":"Oteo, Iván"},{"first_name":"Ian","last_name":"Smail","full_name":"Smail, Ian"},{"full_name":"Morabito, Leah","last_name":"Morabito","first_name":"Leah"},{"first_name":"Ana","last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana"}],"type":"journal_article","date_updated":"2024-10-14T11:35:37Z","day":"01","language":[{"iso":"eng"}],"date_published":"2017-04-01T00:00:00Z","volume":466,"page":"1242-1258","doi":"10.1093/mnras/stw3090","article_processing_charge":"No","oa_version":"Preprint","issue":"1","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"lang":"eng","text":"We present the CAlibrating LYMan-α with Hα (CALYMHA) pilot survey and new results on Lyman α (Lyα) selected galaxies at z ∼ 2. We use a custom-built Lyα narrow-band filter at the Isaac Newton Telescope, designed to provide a matched volume coverage to the z = 2.23 Hα HiZELS survey. Here, we present the first results for the COSMOS and UDS fields. Our survey currently reaches a 3σ line flux limit of ∼4 × 10−17 erg s−1 cm−2, and a Lyα luminosity limit of ∼1042.3 erg s−1. We find 188 Lyα emitters over 7.3 × 105 Mpc3, but also find significant numbers of other line-emitting sources corresponding to He II, C III] and C IV emission lines. These sources are important contaminants, and we carefully remove them, unlike most previous studies. We find that the Lyα luminosity function at z = 2.23 is very well described by a Schechter function up to LLy α ≈ 1043 erg s−1 with L∗=1042.59+0.16−0.08 erg s−1, ϕ∗=10−3.09+0.14−0.34 Mpc−3 and α = −1.75 ± 0.25. Above LLy α ≈ 1043 erg s−1, the Lyα luminosity function becomes power-law like, driven by X-ray AGN. We find that Lyα-selected emitters have a high escape fraction of 37 ± 7 per cent, anticorrelated with Lyα luminosity and correlated with Lyα equivalent width. Lyα emitters have ubiquitous large (≈40 kpc) Lyα haloes, ∼2 times larger than their Hα extents. By directly comparing our Lyα and Hα luminosity functions, we find that the global/overall escape fraction of Lyα photons (within a 13 kpc radius) from the full population of star-forming galaxies is 5.1 ± 0.2 per cent at the peak of the star formation history. An extra 3.3 ± 0.3 per cent of Lyα photons likely still escape, but at larger radii."}],"status":"public"},{"citation":{"mla":"Matthee, Jorryt J., et al. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 3, Oxford University Press, 2017, pp. 3637–55, doi:<a href=\"https://doi.org/10.1093/mnras/stw2973\">10.1093/mnras/stw2973</a>.","chicago":"Matthee, Jorryt J, David Sobral, Philip Best, Ali Ahmad Khostovan, Iván Oteo, Rychard Bouwens, and Huub Röttgering. “The Production and Escape of Lyman-Continuum Radiation from Star-Forming Galaxies at z ∼ 2 and Their Redshift Evolution.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2973\">https://doi.org/10.1093/mnras/stw2973</a>.","ieee":"J. J. Matthee <i>et al.</i>, “The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 3. Oxford University Press, pp. 3637–3655, 2017.","ama":"Matthee JJ, Sobral D, Best P, et al. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(3):3637-3655. doi:<a href=\"https://doi.org/10.1093/mnras/stw2973\">10.1093/mnras/stw2973</a>","apa":"Matthee, J. J., Sobral, D., Best, P., Khostovan, A. A., Oteo, I., Bouwens, R., &#38; Röttgering, H. (2017). The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2973\">https://doi.org/10.1093/mnras/stw2973</a>","ista":"Matthee JJ, Sobral D, Best P, Khostovan AA, Oteo I, Bouwens R, Röttgering H. 2017. The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution. Monthly Notices of the Royal Astronomical Society. 465(3), 3637–3655.","short":"J.J. Matthee, D. Sobral, P. Best, A.A. Khostovan, I. Oteo, R. Bouwens, H. Röttgering, Monthly Notices of the Royal Astronomical Society 465 (2017) 3637–3655."},"title":"The production and escape of Lyman-Continuum radiation from star-forming galaxies at z ∼ 2 and their redshift evolution","quality_controlled":"1","main_file_link":[{"url":"https://arxiv.org/abs/1605.08782","open_access":"1"}],"date_created":"2022-07-12T12:12:14Z","extern":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11564","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"external_id":{"arxiv":["1605.08782"]},"arxiv":1,"year":"2017","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","cosmology: observations","dark ages","reionization","first stars"],"intvolume":"       465","month":"03","oa":1,"scopus_import":"1","article_type":"original","acknowledgement":"We thank the referee for the many helpful and constructive comments which have significantly improved this paper. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). PNB is grateful for support from the UK STFC via grant ST/M001229/1. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. The authors thank Andreas Faisst, Michael Rutkowski and Andreas Sandberg for answering questions related to this work and Daniel Schaerer and Mark Dijkstra for discussions. We acknowledge the work that has been done by both the COSMOS team in assembling such large, state-of-the-art multi-wavelength data set, as this has been crucial for the results presented in this paper. We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY (Jones et al. 2001; Hunter 2007; Van Der Walt, Colbert & Varoquaux 2011) and ASTROPY (Astropy Collaboration et al. 2013) packages, the astronomical imaging tools SEXTRACTOR and SWARP (Bertin & Arnouts 1996;\r\nBertin 2010) and the TOPCAT analysis program (Taylor 2013).","publication_status":"published","publisher":"Oxford University Press","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"full_name":"Sobral, David","last_name":"Sobral","first_name":"David"},{"first_name":"Philip","full_name":"Best, Philip","last_name":"Best"},{"first_name":"Ali Ahmad","full_name":"Khostovan, Ali Ahmad","last_name":"Khostovan"},{"first_name":"Iván","full_name":"Oteo, Iván","last_name":"Oteo"},{"first_name":"Rychard","full_name":"Bouwens, Rychard","last_name":"Bouwens"},{"first_name":"Huub","last_name":"Röttgering","full_name":"Röttgering, Huub"}],"type":"journal_article","date_updated":"2024-10-14T11:35:49Z","day":"01","date_published":"2017-03-01T00:00:00Z","language":[{"iso":"eng"}],"volume":465,"page":"3637-3655","doi":"10.1093/mnras/stw2973","article_processing_charge":"No","oa_version":"Preprint","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"We study the production rate of ionizing photons of a sample of 588 Hα emitters (HAEs) and 160 Lyman-α emitters (LAEs) at z = 2.2 in the COSMOS field in order to assess the implied emissivity from galaxies, based on their ultraviolet (UV) luminosity. By exploring the rest-frame Lyman Continuum (LyC) with GALEX/NUV data, we find fesc < 2.8 (6.4) per cent through median (mean) stacking. By combining the Hα luminosity density with intergalactic medium emissivity measurements from absorption studies, we find a globally averaged 〈fesc〉 of 5.9+14.5−4.2 per cent at z = 2.2 if we assume HAEs are the only source of ionizing photons. We find similarly low values of the global 〈fesc〉 at z ≈ 3–5, also ruling out a high 〈fesc〉 at z < 5. These low escape fractions allow us to measure ξion, the number of produced ionizing photons per unit UV luminosity, and investigate how this depends on galaxy properties. We find a typical ξion ≈ 1024.77 ± 0.04 Hz erg−1 for HAEs and ξion ≈ 1025.14 ± 0.09 Hz erg−1 for LAEs. LAEs and low-mass HAEs at z = 2.2 show similar values of ξion as typically assumed in the reionization era, while the typical HAE is three times less ionizing. Due to an increasing ξion with increasing EW(Hα), ξion likely increases with redshift. This evolution alone is fully in line with the observed evolution of ξion between z ≈ 2 and 5, indicating a typical value of ξion ≈ 1025.4 Hz erg−1 in the reionization era.","lang":"eng"}],"status":"public"},{"month":"02","article_type":"original","scopus_import":"1","oa":1,"acknowledgement":"We thank the anonymous referee for their comments. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. JM thanks David Sobral for useful discussions and help with fitting routines and Jonas Chavez Montero and Ying Zu for providing data. We thank PRACE for the access to the Curie facility in France. We have used the DiRAC system which is a part of National E-Infrastructure at Durham University, operated by the Institute for Computational Cosmology on behalf of the STFC DiRAC HPC Facility (www.dirac.ac.uk); the equipment was funded by BIS National E-infrastructure capital grant ST/K00042X/1, STFC capital grant ST/H008519/1, STFC DiRAC Operations grant ST/K003267/1 and Durham University. The study was sponsored by the Dutch National Computing Facilities Foundation (NCF) for the use of supercomputer facilities, with financial support from the Netherlands Organisation for Scientific Research (NWO), through VICI grant 639.043.409, and the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC Grant agreement 278594- GasAroundGalaxies, and from the Belgian Science Policy Office ([AP P7/08 CHARM]). We have benefited greatly from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY, H5PY and RPY2 packages, and the TOPCAT analysis program (Taylor 2005).","publication_status":"published","year":"2017","arxiv":1,"external_id":{"arxiv":["1608.08218"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: formation","galaxies: haloes","cosmology: theory"],"intvolume":"       465","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11565","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"citation":{"ama":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(2):2381-2396. doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>","apa":"Matthee, J. J., Schaye, J., Crain, R. A., Schaller, M., Bower, R., &#38; Theuns, T. (2017). The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>","short":"J.J. Matthee, J. Schaye, R.A. Crain, M. Schaller, R. Bower, T. Theuns, Monthly Notices of the Royal Astronomical Society 465 (2017) 2381–2396.","ista":"Matthee JJ, Schaye J, Crain RA, Schaller M, Bower R, Theuns T. 2017. The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation. Monthly Notices of the Royal Astronomical Society. 465(2), 2381–2396.","mla":"Matthee, Jorryt J., et al. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2, Oxford University Press, 2017, pp. 2381–96, doi:<a href=\"https://doi.org/10.1093/mnras/stw2884\">10.1093/mnras/stw2884</a>.","ieee":"J. J. Matthee, J. Schaye, R. A. Crain, M. Schaller, R. Bower, and T. Theuns, “The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 2. Oxford University Press, pp. 2381–2396, 2017.","chicago":"Matthee, Jorryt J, Joop Schaye, Robert A. Crain, Matthieu Schaller, Richard Bower, and Tom Theuns. “The Origin of Scatter in the Stellar Mass–Halo Mass Relation of Central Galaxies in the EAGLE Simulation.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2884\">https://doi.org/10.1093/mnras/stw2884</a>."},"quality_controlled":"1","title":"The origin of scatter in the stellar mass–halo mass relation of central galaxies in the EAGLE simulation","extern":"1","date_created":"2022-07-12T12:25:08Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1608.08218"}],"oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","issue":"2","status":"public","abstract":[{"lang":"eng","text":"We use the hydrodynamical EAGLE simulation to study the magnitude and origin of the scatter in the stellar mass–halo mass relation for central galaxies. We separate cause and effect by correlating stellar masses in the baryonic simulation with halo properties in a matched dark matter only (DMO) simulation. The scatter in stellar mass increases with redshift and decreases with halo mass. At z = 0.1, it declines from 0.25 dex at M200, DMO ≈ 1011 M⊙ to 0.12 dex at M200, DMO ≈ 1013 M⊙, but the trend is weak above 1012 M⊙. For M200, DMO < 1012.5 M⊙ up to 0.04 dex of the scatter is due to scatter in the halo concentration. At fixed halo mass, a larger stellar mass corresponds to a more concentrated halo. This is likely because higher concentrations imply earlier formation times and hence more time for accretion and star formation, and/or because feedback is less efficient in haloes with higher binding energies. The maximum circular velocity, Vmax, DMO, and binding energy are therefore more fundamental properties than halo mass, meaning that they are more accurate predictors of stellar mass, and we provide fitting formulae for their relations with stellar mass. However, concentration alone cannot explain the total scatter in the Mstar−M200,DMO relation, and it does not explain the scatter in Mstar–Vmax, DMO. Halo spin, sphericity, triaxiality, substructure and environment are also not responsible for the remaining scatter, which thus could be due to more complex halo properties or non-linear/stochastic baryonic effects."}],"language":[{"iso":"eng"}],"date_published":"2017-02-01T00:00:00Z","volume":465,"article_processing_charge":"No","doi":"10.1093/mnras/stw2884","page":"2381-2396","date_updated":"2024-10-14T11:36:05Z","day":"01","author":[{"orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J"},{"last_name":"Schaye","full_name":"Schaye, Joop","first_name":"Joop"},{"first_name":"Robert A.","last_name":"Crain","full_name":"Crain, Robert A."},{"full_name":"Schaller, Matthieu","last_name":"Schaller","first_name":"Matthieu"},{"first_name":"Richard","last_name":"Bower","full_name":"Bower, Richard"},{"first_name":"Tom","full_name":"Theuns, Tom","last_name":"Theuns"}],"publisher":"Oxford University Press","type":"journal_article"},{"month":"11","oa":1,"scopus_import":"1","article_type":"original","publication_status":"published","acknowledgement":"We would like to thank the anonymous referee for her/his valuable input that helped improve the clarity and interpretation of our results. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO), through a Veni fellowship. IO acknowledges support from the European Research Council in the form of the Advanced Investigator Programme, 321302, COSMICISM. CALYMHA data are based on observations made with the Isaac Newton Telescope (proposals 13AN002, I14AN002, 088-INT7/14A, I14BN006, 118-INT13/14B, I15AN008) 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 Astrofísica de Canarias. Also based on data products from observations made with ESO Telescopes at the La Silla Paranal Observatory under ESO programme IDs 098.A-0819 and 179.A-2005. We are grateful to E. L. Wright and J. Schombert for their cosmology calculator. We would like to thank the authors of NUMPY (van der Walt et al. 2011), SCIPY (Jones et al. 2001), MATPLOTLIB (Hunter 2007) and ASTROPY (Astropy Collaboration et al. 2013) for making these packages publicly available. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is ","year":"2017","external_id":{"arxiv":["1703.10169"]},"arxiv":1,"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high-redshift","quasars: emission lines","galaxies: star formation","cosmology: observations"],"intvolume":"       471","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11566","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"citation":{"ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2558–2574, 2017.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, Morphologies and Equivalent Widths .” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2558–74, doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>.","short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2558–2574.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . Monthly Notices of the Royal Astronomical Society. 471(3), 2558–2574.","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1712\">https://doi.org/10.1093/mnras/stx1712</a>","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths . <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2558-2574. doi:<a href=\"https://doi.org/10.1093/mnras/stx1712\">10.1093/mnras/stx1712</a>"},"quality_controlled":"1","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – I. Nature, morphologies and equivalent widths ","extern":"1","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1703.10169"}],"date_created":"2022-07-12T12:33:16Z","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","issue":"3","status":"public","abstract":[{"text":"While traditionally associated with active galactic nuclei (AGN), the properties of the C II] (λ = 2326 Å), C III] (λ, λ = 1907, 1909 Å) and C IV (λ, λ = 1549, 1551 Å) emission lines are still uncertain as large, unbiased samples of sources are scarce. We present the first blind, statistical study of C II], C III] and C IV emitters at z ∼ 0.68, 1.05, 1.53, respectively, uniformly selected down to a flux limit of ∼4 × 10−17 erg s−1 cm−1 through a narrow-band survey covering an area of ∼1.4 deg2 over COSMOS and UDS. We detect 16 C II], 35 C III] and 17 C IV emitters, whose nature we investigate using optical colours as well as Hubble Space Telescope (HST), X-ray, radio and far-infrared data. We find that z ∼ 0.7 C II] emitters are consistent with a mixture of blue (UV slope β = −2.0 ± 0.4) star-forming (SF) galaxies with discy HST structure and AGN with Seyfert-like morphologies. Bright C II] emitters have individual X-ray detections as well as high average black hole accretion rates (BHARs) of ∼0.1 M⊙ yr−1. C III] emitters at z ∼ 1.05 trace a general population of SF galaxies, with β = −0.8 ± 1.1, a variety of optical morphologies, including isolated and interacting galaxies and low BHAR (<0.02 M⊙ yr−1). Our C IV emitters at z ∼ 1.5 are consistent with young, blue quasars (β ∼ −1.9) with point-like optical morphologies, bright X-ray counterparts and large BHAR (0.8  M⊙ yr−1). We also find some surprising C II], C III] and C IV emitters with rest-frame equivalent widths (EWs) that could be as large as 50–100 Å. AGN or spatial offsets between the UV continuum stellar disc and the line-emitting regions may explain the large EW. These bright C II], C III] and C IV emitters are ideal candidates for spectroscopic follow-up to fully unveil their nature.","lang":"eng"}],"language":[{"iso":"eng"}],"date_published":"2017-11-01T00:00:00Z","volume":471,"doi":"10.1093/mnras/stx1712","article_processing_charge":"No","page":"2558-2574","date_updated":"2022-08-19T07:59:57Z","day":"01","publisher":"Oxford University Press","author":[{"first_name":"Andra","last_name":"Stroe","full_name":"Stroe, Andra"},{"first_name":"David","last_name":"Sobral","full_name":"Sobral, David"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J","orcid":"0000-0003-2871-127X"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"first_name":"Ivan","last_name":"Oteo","full_name":"Oteo, Ivan"}],"type":"journal_article"},{"citation":{"short":"A. Stroe, D. Sobral, J.J. Matthee, J. Calhau, I. Oteo, Monthly Notices of the Royal Astronomical Society 471 (2017) 2575–2586.","ista":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. 2017. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. Monthly Notices of the Royal Astronomical Society. 471(3), 2575–2586.","ama":"Stroe A, Sobral D, Matthee JJ, Calhau J, Oteo I. A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(3):2575-2586. doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>","apa":"Stroe, A., Sobral, D., Matthee, J. J., Calhau, J., &#38; Oteo, I. (2017). A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>","ieee":"A. Stroe, D. Sobral, J. J. Matthee, J. Calhau, and I. Oteo, “A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3. Oxford University Press, pp. 2575–2586, 2017.","chicago":"Stroe, Andra, David Sobral, Jorryt J Matthee, João Calhau, and Ivan Oteo. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1713\">https://doi.org/10.1093/mnras/stx1713</a>.","mla":"Stroe, Andra, et al. “A 1.4 Deg2 Blind Survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity Functions and Cosmic Average Line Ratios.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 3, Oxford University Press, 2017, pp. 2575–86, doi:<a href=\"https://doi.org/10.1093/mnras/stx1713\">10.1093/mnras/stx1713</a>."},"quality_controlled":"1","title":"A 1.4 deg2 blind survey for C II], C III] and C IV at z ∼ 0.7–1.5 – II. Luminosity functions and cosmic average line ratios","extern":"1","main_file_link":[{"url":"https://arxiv.org/abs/1703.10169","open_access":"1"}],"date_created":"2022-07-12T12:54:57Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11567","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"year":"2017","arxiv":1,"external_id":{"arxiv":["1703.10169"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: active","galaxies: high redshift","galaxies: luminosity function","mass function","quasars: emission lines","star formation","cosmology: observations"],"intvolume":"       471","month":"11","oa":1,"scopus_import":"1","article_type":"original","publication_status":"published","publisher":"Oxford University Press","author":[{"first_name":"Andra","full_name":"Stroe, Andra","last_name":"Stroe"},{"first_name":"David","full_name":"Sobral, David","last_name":"Sobral"},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Calhau","full_name":"Calhau, João","first_name":"João"},{"last_name":"Oteo","full_name":"Oteo, Ivan","first_name":"Ivan"}],"type":"journal_article","date_updated":"2022-08-19T08:02:04Z","day":"01","date_published":"2017-11-01T00:00:00Z","language":[{"iso":"eng"}],"volume":471,"doi":"10.1093/mnras/stx1713","article_processing_charge":"No","page":"2575-2586","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","issue":"3","status":"public","abstract":[{"lang":"eng","text":"Recently, the C III] and C IV emission lines have been observed in galaxies in the early Universe (z > 5), providing new ways to measure their redshift and study their stellar populations and active galactic nuclei (AGN). We explore the first blind C II], C III] and C IV survey (z ∼ 0.68, 1.05, 1.53, respectively) presented in Stroe et al. (2017). We derive luminosity functions (LF) and study properties of C II], C III] and C IV line emitters through comparisons to the LFs of H α and Ly α emitters, UV selected star-forming (SF) galaxies and quasars at similar redshifts. The C II] LF at z ∼ 0.68 is equally well described by a Schechter or a power-law LF, characteristic of a mixture of SF and AGN activity. The C III] LF (z ∼ 1.05) is consistent to a scaled down version of the Schechter H α and Ly α LF at their redshift, indicating a SF origin. In stark contrast, the C IV LF at z ∼ 1.53 is well fit by a power-law, quasar-like LF. We find that the brightest UV sources (MUV < −22) will universally have C III] and C IV emission. However, on average, C III] and C IV are not as abundant as H α or Ly α emitters at the same redshift, with cosmic average ratios of ∼0.02–0.06 to H α and ∼0.01–0.1 to intrinsic Ly α. We predict that the C III] and C IV lines can only be truly competitive in confirming high-redshift candidates when the hosts are intrinsically bright and the effective Ly α escape fraction is below 1 per cent. While C III] and C IV were proposed as good tracers of young, relatively low-metallicity galaxies typical of the early Universe, we find that, at least at z ∼ 1.5, C IV is exclusively hosted by AGN/quasars, especially at large line equivalent widths."}]},{"oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","status":"public","abstract":[{"lang":"eng","text":"We present spectroscopic follow-up of candidate luminous Ly α emitters (LAEs) at z = 5.7–6.6 in the SA22 field with VLT/X-SHOOTER. We confirm two new luminous LAEs at z = 5.676 (SR6) and z = 6.532 (VR7), and also present HST follow-up of both sources. These sources have luminosities LLy α ≈ 3 × 1043 erg s−1, very high rest-frame equivalent widths of EW0 ≳ 200 Å and narrow Ly α lines (200–340 km s−1). VR7 is the most UV-luminous LAE at z > 6.5, with M1500 = −22.5, even brighter in the UV than CR7. Besides Ly α, we do not detect any other rest-frame UV lines in the spectra of SR6 and VR7, and argue that rest-frame UV lines are easier to observe in bright galaxies with low Ly α equivalent widths. We confirm that Ly α line widths increase with Ly α luminosity at z = 5.7, while there are indications that Ly α lines of faint LAEs become broader at z = 6.6, potentially due to reionization. We find a large spread of up to 3 dex in UV luminosity for >L⋆ LAEs, but find that the Ly α luminosity of the brightest LAEs is strongly related to UV luminosity at z = 6.6. Under basic assumptions, we find that several LAEs at z ≈ 6–7 have Ly α escape fractions ≳ 100  per cent, indicating bursty star formation histories, alternative Ly α production mechanisms, or dust attenuating Ly α emission differently than UV emission. Finally, we present a method to compute ξion, the production efficiency of ionizing photons, and find that LAEs at z ≈ 6–7 have high values of log10(ξion/Hz erg−1) ≈ 25.51 ± 0.09 that may alleviate the need for high Lyman-Continuum escape fractions required for reionization."}],"language":[{"iso":"eng"}],"date_published":"2017-11-01T00:00:00Z","volume":472,"doi":"10.1093/mnras/stx2061","article_processing_charge":"No","page":"772-787","date_updated":"2024-10-14T11:36:26Z","day":"01","author":[{"last_name":"Matthee","full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Sobral","full_name":"Sobral, David","first_name":"David"},{"first_name":"Behnam","last_name":"Darvish","full_name":"Darvish, Behnam"},{"first_name":"Sérgio","last_name":"Santos","full_name":"Santos, Sérgio"},{"last_name":"Mobasher","full_name":"Mobasher, Bahram","first_name":"Bahram"},{"last_name":"Paulino-Afonso","full_name":"Paulino-Afonso, Ana","first_name":"Ana"},{"first_name":"Huub","full_name":"Röttgering, Huub","last_name":"Röttgering"},{"first_name":"Lara","last_name":"Alegre","full_name":"Alegre, Lara"}],"publisher":"Oxford University Press","type":"journal_article","month":"11","oa":1,"article_type":"original","scopus_import":"1","acknowledgement":"We thank the referee for a constructive report that has improved the quality and clarity of this work. The authors thank Grecco Oyarzún for discussions. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organisation for Scientific research (NWO) through a Veni fellowship and from Lancaster University through an Early Career Internal Grant A100679. BD acknowledges financial support from NASA through the Astrophysics Data Analysis Program (ADAP), grant number NNX12AE20G. We thank Kasper Schmidt for providing measurements. Based on observations with the W.M. Keck Observatory through programme C267D. The W.M. Keck Observatory is operated as a scientific partnership amongst the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. Based on observations made with ESO Telescopes at the La Silla Paranal Observatory under programme IDs 097.A-0943, 294.A 5018 and 098.A-0819 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 observing time (W16AN004) and 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. Based on observations made with the NASA/ESA HST, obtained (from the Data Archive) at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with programme #14699. We are grateful for the excellent data sets from the COSMOS, UltraVISTA, SXDS, UDS and CFHTLS survey teams; without these legacy surveys, this research would have been impossible. We have benefited from the public available programming language PYTHON, including the NUMPY, MATPLOTLIB, PYFITS, SCIPY and ASTROPY packages, the astronomical imaging tools SEXTRACTOR, SWARP and SCAMP and the TOPCAT analysis tool (Taylor 2013).","publication_status":"published","year":"2017","arxiv":1,"external_id":{"arxiv":["1706.06591"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution – galaxies: high-redshift","dark ages","reionization","first stars","cosmology: observations"],"intvolume":"       472","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11572","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"short":"J.J. Matthee, D. Sobral, B. Darvish, S. Santos, B. Mobasher, A. Paulino-Afonso, H. Röttgering, L. Alegre, Monthly Notices of the Royal Astronomical Society 472 (2017) 772–787.","ista":"Matthee JJ, Sobral D, Darvish B, Santos S, Mobasher B, Paulino-Afonso A, Röttgering H, Alegre L. 2017. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. Monthly Notices of the Royal Astronomical Society. 472(1), 772–787.","ama":"Matthee JJ, Sobral D, Darvish B, et al. Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;472(1):772-787. doi:<a href=\"https://doi.org/10.1093/mnras/stx2061\">10.1093/mnras/stx2061</a>","apa":"Matthee, J. J., Sobral, D., Darvish, B., Santos, S., Mobasher, B., Paulino-Afonso, A., … Alegre, L. (2017). Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx2061\">https://doi.org/10.1093/mnras/stx2061</a>","ieee":"J. J. Matthee <i>et al.</i>, “Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 472, no. 1. Oxford University Press, pp. 772–787, 2017.","chicago":"Matthee, Jorryt J, David Sobral, Behnam Darvish, Sérgio Santos, Bahram Mobasher, Ana Paulino-Afonso, Huub Röttgering, and Lara Alegre. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx2061\">https://doi.org/10.1093/mnras/stx2061</a>.","mla":"Matthee, Jorryt J., et al. “Spectroscopic Properties of Luminous Ly α Emitters at z ≈ 6–7 and Comparison to the Lyman-Break Population.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 472, no. 1, Oxford University Press, 2017, pp. 772–87, doi:<a href=\"https://doi.org/10.1093/mnras/stx2061\">10.1093/mnras/stx2061</a>."},"quality_controlled":"1","title":"Spectroscopic properties of luminous Ly α emitters at z ≈ 6–7 and comparison to the Lyman-break population","extern":"1","date_created":"2022-07-13T09:47:39Z","main_file_link":[{"open_access":"1","url":"https://arxiv.org/abs/1706.06591"}]},{"day":"01","date_updated":"2022-08-19T08:07:31Z","type":"journal_article","author":[{"full_name":"Turner, O. J.","last_name":"Turner","first_name":"O. J."},{"full_name":"Cirasuolo, M.","last_name":"Cirasuolo","first_name":"M."},{"last_name":"Harrison","full_name":"Harrison, C. M.","first_name":"C. M."},{"last_name":"McLure","full_name":"McLure, R. J.","first_name":"R. J."},{"last_name":"Dunlop","full_name":"Dunlop, J. S.","first_name":"J. S."},{"first_name":"A. M.","full_name":"Swinbank, A. M.","last_name":"Swinbank"},{"first_name":"H. L.","last_name":"Johnson","full_name":"Johnson, H. L."},{"full_name":"Sobral, D.","last_name":"Sobral","first_name":"D."},{"full_name":"Matthee, Jorryt J","last_name":"Matthee","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X"},{"last_name":"Sharples","full_name":"Sharples, R. M.","first_name":"R. M."}],"publisher":"Oxford University Press","issue":"2","publication":"Monthly Notices of the Royal Astronomical Society","abstract":[{"text":"We present dynamical measurements from the KMOS (K-band multi-object spectrograph) Deep Survey (KDS), which comprises 77 typical star-forming galaxies at z ≃ 3.5 in the mass range 9.0 < log (M⋆/M⊙) < 10.5. These measurements constrain the internal dynamics, the intrinsic velocity dispersions (σint) and rotation velocities (VC) of galaxies in the high-redshift Universe. The mean velocity dispersion of the galaxies in our sample is σint=70.8+3.3−3.1kms−1⁠, revealing that the increasing average σint with increasing redshift, reported for z ≲ 2, continues out to z ≃ 3.5. Only 36 ± 8 per cent of our galaxies are rotation-dominated (VC/σint > 1), with the sample average VC/σint value much smaller than at lower redshift. After carefully selecting comparable star-forming samples at multiple epochs, we find that the rotation-dominated fraction evolves with redshift with a z−0.2 dependence. The rotation-dominated KDS galaxies show no clear offset from the local rotation velocity–stellar mass (i.e. VC–M⋆) relation, although a smaller fraction of the galaxies are on the relation due to the increase in the dispersion-dominated fraction. These observations are consistent with a simple equilibrium model picture, in which random motions are boosted in high-redshift galaxies by a combination of the increasing gas fractions, accretion efficiency, specific star formation rate and stellar feedback and which may provide significant pressure support against gravity on the galactic disc scale.","lang":"eng"}],"status":"public","oa_version":"Preprint","volume":471,"page":"1280-1320","article_processing_charge":"No","doi":"10.1093/mnras/stx1366","language":[{"iso":"eng"}],"date_published":"2017-10-01T00:00:00Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"11573","title":"The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5","quality_controlled":"1","date_created":"2022-07-13T10:03:01Z","main_file_link":[{"url":"https://arxiv.org/abs/1704.06263","open_access":"1"}],"extern":"1","citation":{"mla":"Turner, O. J., et al. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2, Oxford University Press, 2017, pp. 1280–320, doi:<a href=\"https://doi.org/10.1093/mnras/stx1366\">10.1093/mnras/stx1366</a>.","chicago":"Turner, O. J., M. Cirasuolo, C. M. Harrison, R. J. McLure, J. S. Dunlop, A. M. Swinbank, H. L. Johnson, D. Sobral, Jorryt J Matthee, and R. M. Sharples. “The KMOS Deep Survey (KDS) – I. Dynamical Measurements of Typical Star-Forming Galaxies at z ≃ 3.5.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1366\">https://doi.org/10.1093/mnras/stx1366</a>.","ieee":"O. J. Turner <i>et al.</i>, “The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2. Oxford University Press, pp. 1280–1320, 2017.","ama":"Turner OJ, Cirasuolo M, Harrison CM, et al. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(2):1280-1320. doi:<a href=\"https://doi.org/10.1093/mnras/stx1366\">10.1093/mnras/stx1366</a>","apa":"Turner, O. J., Cirasuolo, M., Harrison, C. M., McLure, R. J., Dunlop, J. S., Swinbank, A. M., … Sharples, R. M. (2017). The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1366\">https://doi.org/10.1093/mnras/stx1366</a>","ista":"Turner OJ, Cirasuolo M, Harrison CM, McLure RJ, Dunlop JS, Swinbank AM, Johnson HL, Sobral D, Matthee JJ, Sharples RM. 2017. The KMOS Deep Survey (KDS) – I. Dynamical measurements of typical star-forming galaxies at z ≃ 3.5. Monthly Notices of the Royal Astronomical Society. 471(2), 1280–1320.","short":"O.J. Turner, M. Cirasuolo, C.M. Harrison, R.J. McLure, J.S. Dunlop, A.M. Swinbank, H.L. Johnson, D. Sobral, J.J. Matthee, R.M. Sharples, Monthly Notices of the Royal Astronomical Society 471 (2017) 1280–1320."},"scopus_import":"1","oa":1,"article_type":"original","publication_status":"published","acknowledgement":"We wish to thank the anonymous referee for their comments, which have improved the quality and clarity of this work. OJT acknowledges the financial support of the Science and Technology Facilities Council through a studentship award. MC and OJT acknowledge the KMOS team and all the personnel of the European Southern Observatory Very Large Telescope for outstanding support during the KMOS GTO observations. CMH, AMS and RMS acknowledge the Science and Technology Facilities Council through grant code ST/L00075X/1. RJM acknowledges the support of the European Research Council via the award of a Consolidator Grant (PI: McLure). JSD acknowledges the support of the European Research Council via the award of an Advanced Grant (PI J. Dunlop), and the contribution of the EC FP7 SPACE project ASTRODEEP (Ref.No: 312725). AMS acknowledges the Leverhulme Foundation. JM acknowledges the support of a Huygens PhD fellowship from Leiden University. DS acknowledges financial support from the Netherlands Organization for Scientific research (NWO) through a Veni fellowship and from FCT through an FCT Investigator Starting Grant and Start-up Grant (IF/01154/2012/CP0189/CT0010). This work is based on observations taken by the CANDELS Multi-Cycle Treasury Program with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. This work is based on observations taken by the 3D HST Treasury Program (GO 12177 and 12328) with the NASA/ESA HST, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5-26555. Based on data obtained with the European Southern Observatory Very Large Telescope, Paranal, Chile, under Large Program 185.A-0791, and made available by the VUDS team at the CESAM data centre, Laboratoire d’Astrophysique de Marseille, France. Based on observations obtained at the Very Large Telescope of the European Southern Observatory. Programme IDs: 092.A 0399(A), 093.A-0122(A,B), 094.A-0214(A,B),095.A0680(A,B),096.A-0315(A,B,C).","month":"10","keyword":["Space and Planetary Science","Astronomy and Astrophysics","galaxies: evolution","galaxies: high-redshift","galaxies: kinematics and dynamics"],"intvolume":"       471","arxiv":1,"external_id":{"arxiv":["1704.06263"]},"year":"2017"},{"month":"10","scopus_import":"1","oa":1,"article_type":"original","publication_status":"published","year":"2017","arxiv":1,"external_id":{"arxiv":["1709.08097"]},"keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"intvolume":"       474","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","_id":"15239","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"citation":{"short":"A. Obertas, I. Caiazzo, J. Heyl, H. Richer, J. Kalirai, P.-E. Tremblay, Monthly Notices of the Royal Astronomical Society 474 (2017) 677–682.","ista":"Obertas A, Caiazzo I, Heyl J, Richer H, Kalirai J, Tremblay P-E. 2017. The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae. Monthly Notices of the Royal Astronomical Society. 474(1), 677–682.","apa":"Obertas, A., Caiazzo, I., Heyl, J., Richer, H., Kalirai, J., &#38; Tremblay, P.-E. (2017). The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx2759\">https://doi.org/10.1093/mnras/stx2759</a>","ama":"Obertas A, Caiazzo I, Heyl J, Richer H, Kalirai J, Tremblay P-E. The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;474(1):677-682. doi:<a href=\"https://doi.org/10.1093/mnras/stx2759\">10.1093/mnras/stx2759</a>","ieee":"A. Obertas, I. Caiazzo, J. Heyl, H. Richer, J. Kalirai, and P.-E. Tremblay, “The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 474, no. 1. Oxford University Press, pp. 677–682, 2017.","chicago":"Obertas, Alysa, Ilaria Caiazzo, Jeremy Heyl, Harvey Richer, Jason Kalirai, and Pier-Emmanuel Tremblay. “The Onset of Convective Coupling and Freezing in the White Dwarfs of 47 Tucanae.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx2759\">https://doi.org/10.1093/mnras/stx2759</a>.","mla":"Obertas, Alysa, et al. “The Onset of Convective Coupling and Freezing in the White Dwarfs of 47 Tucanae.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 474, no. 1, Oxford University Press, 2017, pp. 677–82, doi:<a href=\"https://doi.org/10.1093/mnras/stx2759\">10.1093/mnras/stx2759</a>."},"quality_controlled":"1","title":"The onset of convective coupling and freezing in the white dwarfs of 47 Tucanae","extern":"1","date_created":"2024-03-26T10:40:05Z","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.1709.08097","open_access":"1"}],"oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","status":"public","abstract":[{"lang":"eng","text":"Using images from the Hubble Space Telescope Advanced Camera for Surveys, we measure the rate of cooling of white dwarfs in the globular cluster 47 Tucanae and compare it to modelled cooling curves. We examine the effects of the outer convective envelope reaching the nearly isothermal degenerate core and the release of latent heat during core crystallization on the white dwarf cooling rates. For white dwarfs typical of 47 Tuc, the onset of these effects occur at similar times. The latent heat released during crystallization is a small heat source. In contrast, the heat reservoir of the degenerate core is substantially larger. When the convective envelope reaches the nearly isothermal interior of the white dwarf, the star becomes brighter than it would be in the absence of this effect. Our modelled cooling curves that include this convective coupling closely match the observed luminosity function of the white dwarfs in 47 Tuc."}],"date_published":"2017-10-24T00:00:00Z","language":[{"iso":"eng"}],"volume":474,"doi":"10.1093/mnras/stx2759","article_processing_charge":"No","page":"677-682","date_updated":"2024-04-08T07:04:10Z","day":"24","author":[{"last_name":"Obertas","full_name":"Obertas, Alysa","first_name":"Alysa"},{"last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d"},{"last_name":"Heyl","full_name":"Heyl, Jeremy","first_name":"Jeremy"},{"last_name":"Richer","full_name":"Richer, Harvey","first_name":"Harvey"},{"first_name":"Jason","last_name":"Kalirai","full_name":"Kalirai, Jason"},{"first_name":"Pier-Emmanuel","full_name":"Tremblay, Pier-Emmanuel","last_name":"Tremblay"}],"publisher":"Oxford University Press","type":"journal_article"},{"author":[{"last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria","orcid":"0000-0002-4770-5388"},{"last_name":"Heyl","full_name":"Heyl, Jeremy S.","first_name":"Jeremy S."}],"publisher":"Oxford University Press","type":"journal_article","date_updated":"2024-10-14T12:33:43Z","day":"01","date_published":"2017-05-01T00:00:00Z","language":[{"iso":"eng"}],"page":"2750-2759","article_processing_charge":"No","doi":"10.1093/mnras/stx1036","volume":469,"oa_version":"Preprint","abstract":[{"lang":"eng","text":"We present a model to account for the observed debris discs around young white dwarfs and the presence of metal lines in their spectra. Stellar evolution models predict that the mass-loss on the AGB will be pulsed; furthermore, observations indicate that the bulk of the mass-loss occurs on the AGB. In this case, if the progenitors of the white dwarfs had remnants of planetary formation like the Sun’s Oort cloud or the Kuiper Belt and a planet lying within that cloud or nearby, we find that up to 2 per cent of the planetesimals will fall either into planet-crossing orbits or into chaotic regions after the mass-loss, depending on the location and mass of the planet (from Mars to Neptune). This yields a sufficient mass of comets that can be scattered towards the star, form a debris disc and pollute the atmosphere."}],"status":"public","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","citation":{"ieee":"I. Caiazzo and J. S. Heyl, “Polluting white dwarfs with perturbed exo-comets,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 469, no. 3. Oxford University Press, pp. 2750–2759, 2017.","chicago":"Caiazzo, Ilaria, and Jeremy S. Heyl. “Polluting White Dwarfs with Perturbed Exo-Comets.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1036\">https://doi.org/10.1093/mnras/stx1036</a>.","mla":"Caiazzo, Ilaria, and Jeremy S. Heyl. “Polluting White Dwarfs with Perturbed Exo-Comets.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 469, no. 3, Oxford University Press, 2017, pp. 2750–59, doi:<a href=\"https://doi.org/10.1093/mnras/stx1036\">10.1093/mnras/stx1036</a>.","short":"I. Caiazzo, J.S. Heyl, Monthly Notices of the Royal Astronomical Society 469 (2017) 2750–2759.","ista":"Caiazzo I, Heyl JS. 2017. Polluting white dwarfs with perturbed exo-comets. Monthly Notices of the Royal Astronomical Society. 469(3), 2750–2759.","apa":"Caiazzo, I., &#38; Heyl, J. S. (2017). Polluting white dwarfs with perturbed exo-comets. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1036\">https://doi.org/10.1093/mnras/stx1036</a>","ama":"Caiazzo I, Heyl JS. Polluting white dwarfs with perturbed exo-comets. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;469(3):2750-2759. doi:<a href=\"https://doi.org/10.1093/mnras/stx1036\">10.1093/mnras/stx1036</a>"},"date_created":"2024-03-26T10:40:45Z","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1702.07682"}],"extern":"1","title":"Polluting white dwarfs with perturbed exo-comets","quality_controlled":"1","_id":"15241","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"external_id":{"arxiv":["1702.07682"]},"arxiv":1,"year":"2017","intvolume":"       469","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"month":"05","publication_status":"published","oa":1,"scopus_import":"1","article_type":"original"},{"day":"13","date_updated":"2024-04-08T07:05:47Z","type":"journal_article","publisher":"Oxford University Press","author":[{"first_name":"C.","full_name":"Elenbaas, C.","last_name":"Elenbaas"},{"last_name":"Huppenkothen","full_name":"Huppenkothen, D.","first_name":"D."},{"full_name":"Omand, C.","last_name":"Omand","first_name":"C."},{"first_name":"A. L.","full_name":"Watts, A. L.","last_name":"Watts"},{"last_name":"Bissaldi","full_name":"Bissaldi, E.","first_name":"E."},{"full_name":"Caiazzo, Ilaria","last_name":"Caiazzo","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","orcid":"0000-0002-4770-5388"},{"last_name":"Heyl","full_name":"Heyl, J.","first_name":"J."}],"abstract":[{"text":"High-energy (>250 keV) emission has been detected persisting for several tens of seconds after the initial spike of magnetar giant flares (GFs). It has been conjectured that this emission might arise via inverse Compton scattering in a highly extended corona generated by super-Eddington outflows high up in the magnetosphere. In this paper, we undertake a detailed examination of this model. We investigate the properties of the required scatterers, and whether the mechanism is consistent with the degree of pulsed emission observed in the tail of the GF. We conclude that the mechanism is consistent with current data, although the origin of the scattering population remains an open question. We propose an alternative picture in which the emission is closer to that star and is dominated by synchrotron radiation. The Reuven Ramaty High Energy Solar Spectroscopic Imager observations of the 2004 December flare modestly favour this latter picture. We assess the prospects for the Fermi Gamma-ray Space Telescope to detect and characterize a similar high-energy component in a future GF. Such a detection should help to resolve some of the outstanding issues.","lang":"eng"}],"status":"public","issue":"2","publication":"Monthly Notices of the Royal Astronomical Society","oa_version":"Preprint","page":"1856-1872","article_processing_charge":"No","doi":"10.1093/mnras/stx1727","volume":471,"language":[{"iso":"eng"}],"date_published":"2017-07-13T00:00:00Z","publication_identifier":{"issn":["0035-8711"],"eissn":["1365-2966"]},"_id":"15243","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.1707.02922"}],"date_created":"2024-03-26T10:41:24Z","extern":"1","title":"Magnetar giant flare high-energy emission","quality_controlled":"1","citation":{"mla":"Elenbaas, C., et al. “Magnetar Giant Flare High-Energy Emission.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2, Oxford University Press, 2017, pp. 1856–72, doi:<a href=\"https://doi.org/10.1093/mnras/stx1727\">10.1093/mnras/stx1727</a>.","chicago":"Elenbaas, C., D. Huppenkothen, C. Omand, A. L. Watts, E. Bissaldi, Ilaria Caiazzo, and J. Heyl. “Magnetar Giant Flare High-Energy Emission.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1727\">https://doi.org/10.1093/mnras/stx1727</a>.","ieee":"C. Elenbaas <i>et al.</i>, “Magnetar giant flare high-energy emission,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 471, no. 2. Oxford University Press, pp. 1856–1872, 2017.","ama":"Elenbaas C, Huppenkothen D, Omand C, et al. Magnetar giant flare high-energy emission. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;471(2):1856-1872. doi:<a href=\"https://doi.org/10.1093/mnras/stx1727\">10.1093/mnras/stx1727</a>","apa":"Elenbaas, C., Huppenkothen, D., Omand, C., Watts, A. L., Bissaldi, E., Caiazzo, I., &#38; Heyl, J. (2017). Magnetar giant flare high-energy emission. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1727\">https://doi.org/10.1093/mnras/stx1727</a>","ista":"Elenbaas C, Huppenkothen D, Omand C, Watts AL, Bissaldi E, Caiazzo I, Heyl J. 2017. Magnetar giant flare high-energy emission. Monthly Notices of the Royal Astronomical Society. 471(2), 1856–1872.","short":"C. Elenbaas, D. Huppenkothen, C. Omand, A.L. Watts, E. Bissaldi, I. Caiazzo, J. Heyl, Monthly Notices of the Royal Astronomical Society 471 (2017) 1856–1872."},"publication_status":"published","scopus_import":"1","article_type":"original","oa":1,"month":"07","intvolume":"       471","keyword":["Space and Planetary Science","Astronomy and Astrophysics"],"external_id":{"arxiv":["1707.02922"]},"arxiv":1,"year":"2017"},{"external_id":{"arxiv":["1608.04519"],"isi":["000395170200039"]},"arxiv":1,"year":"2017","intvolume":"       465","month":"01","acknowledgement":"Part of this work has been supported by the 7th Framework Programme for Research of the European Commission, under FETOpen grant number 255827 (CGL Computational Geometry Learning) and ERC advanced grant, URSAT (Understanding Random Systems via Algebraic Topology) number 320422.","publication_status":"published","scopus_import":"1","oa":1,"citation":{"ieee":"P. Pranav <i>et al.</i>, “The topology of the cosmic web in terms of persistent Betti numbers,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 4. Oxford University Press, pp. 4281–4310, 2017.","chicago":"Pranav, Pratyush, Herbert Edelsbrunner, Rien Van De Weygaert, Gert Vegter, Michael Kerber, Bernard Jones, and Mathijs Wintraecken. “The Topology of the Cosmic Web in Terms of Persistent Betti Numbers.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stw2862\">https://doi.org/10.1093/mnras/stw2862</a>.","mla":"Pranav, Pratyush, et al. “The Topology of the Cosmic Web in Terms of Persistent Betti Numbers.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 465, no. 4, Oxford University Press, 2017, pp. 4281–310, doi:<a href=\"https://doi.org/10.1093/mnras/stw2862\">10.1093/mnras/stw2862</a>.","short":"P. Pranav, H. Edelsbrunner, R. Van De Weygaert, G. Vegter, M. Kerber, B. Jones, M. Wintraecken, Monthly Notices of the Royal Astronomical Society 465 (2017) 4281–4310.","ista":"Pranav P, Edelsbrunner H, Van De Weygaert R, Vegter G, Kerber M, Jones B, Wintraecken M. 2017. The topology of the cosmic web in terms of persistent Betti numbers. Monthly Notices of the Royal Astronomical Society. 465(4), 4281–4310.","apa":"Pranav, P., Edelsbrunner, H., Van De Weygaert, R., Vegter, G., Kerber, M., Jones, B., &#38; Wintraecken, M. (2017). The topology of the cosmic web in terms of persistent Betti numbers. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stw2862\">https://doi.org/10.1093/mnras/stw2862</a>","ama":"Pranav P, Edelsbrunner H, Van De Weygaert R, et al. The topology of the cosmic web in terms of persistent Betti numbers. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;465(4):4281-4310. doi:<a href=\"https://doi.org/10.1093/mnras/stw2862\">10.1093/mnras/stw2862</a>"},"date_created":"2018-12-11T11:49:44Z","main_file_link":[{"url":"https://arxiv.org/abs/1608.04519","open_access":"1"}],"title":"The topology of the cosmic web in terms of persistent Betti numbers","department":[{"_id":"HeEd"}],"quality_controlled":"1","_id":"1022","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","publication_identifier":{"issn":["0035-8711"]},"publist_id":"6373","language":[{"iso":"eng"}],"date_published":"2017-01-01T00:00:00Z","page":"4281 - 4310","doi":"10.1093/mnras/stw2862","article_processing_charge":"No","volume":465,"oa_version":"Submitted Version","abstract":[{"lang":"eng","text":"We introduce a multiscale topological description of the Megaparsec web-like cosmic matter distribution. Betti numbers and topological persistence offer a powerful means of describing the rich connectivity structure of the cosmic web and of its multiscale arrangement of matter and galaxies. Emanating from algebraic topology and Morse theory, Betti numbers and persistence diagrams represent an extension and deepening of the cosmologically familiar topological genus measure and the related geometric Minkowski functionals. In addition to a description of the mathematical background, this study presents the computational procedure for computing Betti numbers and persistence diagrams for density field filtrations. The field may be computed starting from a discrete spatial distribution of galaxies or simulation particles. The main emphasis of this study concerns an extensive and systematic exploration of the imprint of different web-like morphologies and different levels of multiscale clustering in the corresponding computed Betti numbers and persistence diagrams. To this end, we use Voronoi clustering models as templates for a rich variety of web-like configurations and the fractal-like Soneira-Peebles models exemplify a range of multiscale configurations. We have identified the clear imprint of cluster nodes, filaments, walls, and voids in persistence diagrams, along with that of the nested hierarchy of structures in multiscale point distributions. We conclude by outlining the potential of persistent topology for understanding the connectivity structure of the cosmic web, in large simulations of cosmic structure formation and in the challenging context of the observed galaxy distribution in large galaxy surveys."}],"status":"public","issue":"4","publication":"Monthly Notices of the Royal Astronomical Society","author":[{"full_name":"Pranav, Pratyush","last_name":"Pranav","first_name":"Pratyush"},{"full_name":"Edelsbrunner, Herbert","last_name":"Edelsbrunner","first_name":"Herbert","id":"3FB178DA-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-9823-6833"},{"full_name":"Van De Weygaert, Rien","last_name":"Van De Weygaert","first_name":"Rien"},{"first_name":"Gert","last_name":"Vegter","full_name":"Vegter, Gert"},{"first_name":"Michael","last_name":"Kerber","full_name":"Kerber, Michael"},{"first_name":"Bernard","last_name":"Jones","full_name":"Jones, Bernard"},{"last_name":"Wintraecken","full_name":"Wintraecken, Mathijs","first_name":"Mathijs","id":"307CFBC8-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-7472-2220"}],"publisher":"Oxford University Press","type":"journal_article","date_updated":"2025-06-04T08:10:31Z","isi":1,"day":"01"},{"citation":{"ieee":"D. J. D’Orazio and Z. Haiman, “Lighthouse in the dust: infrared echoes of periodic emission from massive black hole binaries★,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 470, no. 1. Oxford University Press, pp. 1198–1217, 2017.","chicago":"D’Orazio, Daniel J., and Zoltán Haiman. “Lighthouse in the Dust: Infrared Echoes of Periodic Emission from Massive Black Hole Binaries★.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx1269\">https://doi.org/10.1093/mnras/stx1269</a>.","mla":"D’Orazio, Daniel J., and Zoltán Haiman. “Lighthouse in the Dust: Infrared Echoes of Periodic Emission from Massive Black Hole Binaries★.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 470, no. 1, Oxford University Press, 2017, pp. 1198–217, doi:<a href=\"https://doi.org/10.1093/mnras/stx1269\">10.1093/mnras/stx1269</a>.","short":"D.J. D’Orazio, Z. Haiman, Monthly Notices of the Royal Astronomical Society 470 (2017) 1198–1217.","ista":"D’Orazio DJ, Haiman Z. 2017. Lighthouse in the dust: infrared echoes of periodic emission from massive black hole binaries★. Monthly Notices of the Royal Astronomical Society. 470(1), 1198–1217.","ama":"D’Orazio DJ, Haiman Z. Lighthouse in the dust: infrared echoes of periodic emission from massive black hole binaries★. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;470(1):1198-1217. doi:<a href=\"https://doi.org/10.1093/mnras/stx1269\">10.1093/mnras/stx1269</a>","apa":"D’Orazio, D. J., &#38; Haiman, Z. (2017). Lighthouse in the dust: infrared echoes of periodic emission from massive black hole binaries★. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx1269\">https://doi.org/10.1093/mnras/stx1269</a>"},"extern":"1","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1093/mnras/stx1269"}],"date_created":"2024-09-05T13:32:36Z","quality_controlled":"1","title":"Lighthouse in the dust: infrared echoes of periodic emission from massive black hole binaries★","_id":"17616","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_identifier":{"issn":["0035-8711","1365-2966"]},"year":"2017","intvolume":"       470","month":"05","publication_status":"published","article_type":"original","scopus_import":"1","oa":1,"author":[{"first_name":"Daniel J.","last_name":"D'Orazio","full_name":"D'Orazio, Daniel J."},{"full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"}],"publisher":"Oxford University Press","type":"journal_article","date_updated":"2024-09-24T08:01:52Z","day":"23","date_published":"2017-05-23T00:00:00Z","language":[{"iso":"eng"}],"doi":"10.1093/mnras/stx1269","article_processing_charge":"No","page":"1198-1217","volume":470,"oa_version":"Published Version","status":"public","abstract":[{"lang":"eng","text":"The optical and UV emission from sub-parsec massive black hole binaries (MBHBs) in active galactic nuclei (AGNs) is believed to vary periodically, on time-scales comparable to the binary's orbital time. If driven by accretion rate fluctuations, the variability could be isotropic. If dominated by relativistic Doppler modulation, the variability should instead be anisotropic, resembling a rotating forward-beamed lighthouse. We consider the infrared (IR) reverberation of either type of periodic emission by pc-scale circumbinary dust tori. We predict the phase and amplitude of IR variability as a function of the ratio of dust light crossing time to the source variability period, and of the torus inclination and opening angle. We enumerate several differences between the isotropic and anisotropic cases. Interestingly, for a nearly face-on binary with an inclined dust torus, the Doppler boost can produce IR variability without any observable optical/UV variability. Such orphan-IR variability would have been missed in optical searches for periodic AGNs. We apply our models to time-domain WISE IR data from the MBHB candidate PG 1302−102 and find consistency with dust reverberation by both isotropically emitting and Doppler-boosted sources in the shorter wavelength W1–W2 (2.8 → 5.3 μm) bands. We constrain the dust torus to be thin (aspect ratio ∼ 0.1), with an inner radius at 1–5 pc. More generally, our dust-echo models will aid in identifying new MBHB candidates, determining their nature and constraining the physical properties of MBHBs and their dust tori."}],"publication":"Monthly Notices of the Royal Astronomical Society","issue":"1"},{"oa_version":"Preprint","status":"public","abstract":[{"text":"In symmetric gravitating systems experiencing rapid mass-loss, particle orbits change almost instantaneously, which can lead to the development of a sharply contoured density profile, including singular caustics for collisionless systems. This framework can be used to model a variety of dynamical systems, such as accretion discs following a massive black hole merger and dwarf galaxies following violent early star formation feedback. Particle interactions in the high-density peaks seem a promising source of observable signatures of these mass-loss events (i.e. a possible EM counterpart for black hole mergers or strong gamma-ray emission from dark matter annihilation around young galaxies), because the interaction rate depends on the square of the density. We study post-mass-loss density profiles, both analytic and numerical, in idealized cases and present arguments and methods to extend to any general system. An analytic derivation is presented for particles on Keplerian orbits responding to a drop in the central mass. We argue that this case, with initially circular orbits, gives the most sharply contoured profile possible. We find that despite the presence of a set of singular caustics, the total particle interaction rate is reduced compared to the unperturbed system; this is a result of the overall expansion of the system dominating over the steep caustics. Finally, we argue that this result holds more generally, and the loss of central mass decreases the particle interaction rate in any physical system.","lang":"eng"}],"publication":"Monthly Notices of the Royal Astronomical Society","issue":"1","date_published":"2017-09-25T00:00:00Z","language":[{"iso":"eng"}],"doi":"10.1093/mnras/stx2469","article_processing_charge":"No","page":"498-512","volume":473,"date_updated":"2024-09-24T09:48:08Z","day":"25","publisher":"Oxford University Press","author":[{"first_name":"Zephyr","last_name":"Penoyre","full_name":"Penoyre, Zephyr"},{"id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","first_name":"Zoltán","full_name":"Haiman, Zoltán","last_name":"Haiman"}],"type":"journal_article","month":"09","publication_status":"published","scopus_import":"1","article_type":"original","oa":1,"year":"2017","external_id":{"arxiv":["1709.08640"]},"arxiv":1,"intvolume":"       473","_id":"17630","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_identifier":{"issn":["0035-8711","1365-2966"]},"citation":{"ista":"Penoyre Z, Haiman Z. 2017. A drop in the pond: The effect of rapid mass-loss on the dynamics and interaction rate of collisionless particles. Monthly Notices of the Royal Astronomical Society. 473(1), 498–512.","short":"Z. Penoyre, Z. Haiman, Monthly Notices of the Royal Astronomical Society 473 (2017) 498–512.","ama":"Penoyre Z, Haiman Z. A drop in the pond: The effect of rapid mass-loss on the dynamics and interaction rate of collisionless particles. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;473(1):498-512. doi:<a href=\"https://doi.org/10.1093/mnras/stx2469\">10.1093/mnras/stx2469</a>","apa":"Penoyre, Z., &#38; Haiman, Z. (2017). A drop in the pond: The effect of rapid mass-loss on the dynamics and interaction rate of collisionless particles. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx2469\">https://doi.org/10.1093/mnras/stx2469</a>","chicago":"Penoyre, Zephyr, and Zoltán Haiman. “A Drop in the Pond: The Effect of Rapid Mass-Loss on the Dynamics and Interaction Rate of Collisionless Particles.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx2469\">https://doi.org/10.1093/mnras/stx2469</a>.","ieee":"Z. Penoyre and Z. Haiman, “A drop in the pond: The effect of rapid mass-loss on the dynamics and interaction rate of collisionless particles,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 473, no. 1. Oxford University Press, pp. 498–512, 2017.","mla":"Penoyre, Zephyr, and Zoltán Haiman. “A Drop in the Pond: The Effect of Rapid Mass-Loss on the Dynamics and Interaction Rate of Collisionless Particles.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 473, no. 1, Oxford University Press, 2017, pp. 498–512, doi:<a href=\"https://doi.org/10.1093/mnras/stx2469\">10.1093/mnras/stx2469</a>."},"extern":"1","main_file_link":[{"url":" https://doi.org/10.48550/arXiv.1709.08640","open_access":"1"}],"date_created":"2024-09-05T13:59:48Z","quality_controlled":"1","title":"A drop in the pond: The effect of rapid mass-loss on the dynamics and interaction rate of collisionless particles"},{"publisher":"Oxford University Press","author":[{"last_name":"Leigh","full_name":"Leigh, N W C","first_name":"N W C"},{"first_name":"A M","last_name":"Geller","full_name":"Geller, A M"},{"first_name":"B","full_name":"McKernan, B","last_name":"McKernan"},{"first_name":"K E S","last_name":"Ford","full_name":"Ford, K E S"},{"full_name":"Mac Low, M-M","last_name":"Mac Low","first_name":"M-M"},{"last_name":"Bellovary","full_name":"Bellovary, J","first_name":"J"},{"full_name":"Haiman, Zoltán","last_name":"Haiman","first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36"},{"full_name":"Lyra, W","last_name":"Lyra","first_name":"W"},{"first_name":"J","full_name":"Samsing, J","last_name":"Samsing"},{"first_name":"M","full_name":"O'Dowd, M","last_name":"O'Dowd"},{"last_name":"Kocsis","full_name":"Kocsis, B","first_name":"B"},{"first_name":"S","last_name":"Endlich","full_name":"Endlich, S"}],"type":"journal_article","date_updated":"2024-09-24T10:21:37Z","day":"05","date_published":"2017-12-05T00:00:00Z","language":[{"iso":"eng"}],"volume":474,"article_processing_charge":"No","doi":"10.1093/mnras/stx3134","page":"5672-5683","oa_version":"Preprint","publication":"Monthly Notices of the Royal Astronomical Society","issue":"4","status":"public","abstract":[{"text":"We assess the contribution of dynamical hardening by direct three-body scattering interactions to the rate of stellar-mass black hole binary (BHB) mergers in galactic nuclei. We derive an analytic model for the single-binary encounter rate in a nucleus with spherical and disc components hosting a super-massive black hole (SMBH). We determine the total number of encounters NGW needed to harden a BHB to the point that inspiral due to gravitational wave emission occurs before the next three-body scattering event. This is done independently for both the spherical and disc components. Using a Monte Carlo approach, we refine our calculations for NGW to include gravitational wave emission between scattering events. For astrophysically plausible models, we find that typically NGW ≲ 10. We find two separate regimes for the efficient dynamical hardening of BHBs: (1) spherical star clusters with high central densities, low-velocity dispersions, and no significant Keplerian component and (2) migration traps in discs around SMBHs lacking any significant spherical stellar component in the vicinity of the migration trap, which is expected due to effective orbital inclination reduction of any spherical population by the disc. We also find a weak correlation between the ratio of the second-order velocity moment to velocity dispersion in galactic nuclei and the rate of BHB mergers, where this ratio is a proxy for the ratio between the rotation- and dispersion-supported components. Because discs enforce planar interactions that are efficient in hardening BHBs, particularly in migration traps, they have high merger rates that can contribute significantly to the rate of BHB mergers detected by the advanced Laser Interferometer Gravitational-Wave Observatory.","lang":"eng"}],"citation":{"ama":"Leigh NWC, Geller AM, McKernan B, et al. On the rate of black hole binary mergers in galactic nuclei due to dynamical hardening. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;474(4):5672-5683. doi:<a href=\"https://doi.org/10.1093/mnras/stx3134\">10.1093/mnras/stx3134</a>","apa":"Leigh, N. W. C., Geller, A. M., McKernan, B., Ford, K. E. S., Mac Low, M.-M., Bellovary, J., … Endlich, S. (2017). On the rate of black hole binary mergers in galactic nuclei due to dynamical hardening. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx3134\">https://doi.org/10.1093/mnras/stx3134</a>","ista":"Leigh NWC, Geller AM, McKernan B, Ford KES, Mac Low M-M, Bellovary J, Haiman Z, Lyra W, Samsing J, O’Dowd M, Kocsis B, Endlich S. 2017. On the rate of black hole binary mergers in galactic nuclei due to dynamical hardening. Monthly Notices of the Royal Astronomical Society. 474(4), 5672–5683.","short":"N.W.C. Leigh, A.M. Geller, B. McKernan, K.E.S. Ford, M.-M. Mac Low, J. Bellovary, Z. Haiman, W. Lyra, J. Samsing, M. O’Dowd, B. Kocsis, S. Endlich, Monthly Notices of the Royal Astronomical Society 474 (2017) 5672–5683.","mla":"Leigh, N. W. C., et al. “On the Rate of Black Hole Binary Mergers in Galactic Nuclei Due to Dynamical Hardening.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 474, no. 4, Oxford University Press, 2017, pp. 5672–83, doi:<a href=\"https://doi.org/10.1093/mnras/stx3134\">10.1093/mnras/stx3134</a>.","chicago":"Leigh, N W C, A M Geller, B McKernan, K E S Ford, M-M Mac Low, J Bellovary, Zoltán Haiman, et al. “On the Rate of Black Hole Binary Mergers in Galactic Nuclei Due to Dynamical Hardening.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx3134\">https://doi.org/10.1093/mnras/stx3134</a>.","ieee":"N. W. C. Leigh <i>et al.</i>, “On the rate of black hole binary mergers in galactic nuclei due to dynamical hardening,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 474, no. 4. Oxford University Press, pp. 5672–5683, 2017."},"quality_controlled":"1","title":"On the rate of black hole binary mergers in galactic nuclei due to dynamical hardening","extern":"1","date_created":"2024-09-05T14:16:03Z","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1711.10494"}],"user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","_id":"17632","publication_identifier":{"issn":["0035-8711","1365-2966"]},"year":"2017","arxiv":1,"external_id":{"arxiv":["1711.10494"]},"intvolume":"       474","month":"12","article_type":"original","scopus_import":"1","oa":1,"publication_status":"published"},{"language":[{"iso":"eng"}],"date_published":"2017-09-27T00:00:00Z","page":"3410-3433","doi":"10.1093/mnras/stx2524","article_processing_charge":"No","volume":473,"oa_version":"Preprint","abstract":[{"text":"Using few-body simulations, we investigate the evolution of supermassive black holes (SMBHs) in galaxies (M* = 1010–1012 M⊙ at z = 0) at 0 < z < 4. Following galaxy merger trees from the Millennium simulation, we model BH mergers with two extreme binary decay scenarios for the ‘hard binary’ stage: a full or an empty loss cone. These two models should bracket the true evolution, and allow us to separately explore the role of dynamical friction and that of multibody BH interactions on BH mergers. Using the computed merger rates, we infer the stochastic gravitational wave background (GWB). Our dynamical approach is a first attempt to study the dynamical evolution of multiple SMBHs in the host galaxies undergoing mergers with various mass ratios (10−4 < q* < 1). Our main result demonstrates that SMBH binaries are able to merge in both scenarios. In the empty loss cone case, we find that BHs merge via multibody interactions, avoiding the ‘final parsec’ problem, and entering the pulsar timing arrays band with substantial orbital eccentricity. Our full loss cone treatment, albeit more approximate, suggests that the eccentricity becomes even higher when GWs become dominant, leading to rapid coalescences (binary lifetime ≲1 Gyr). Despite the lower merger rates in the empty loss cone case, due to their higher mass ratios and lower redshifts, the GWB in the full/empty loss cone models are comparable (0.70 × 10−15 and 0.53 × 10−15 at a frequency of 1 yr−1, respectively). Finally, we compute the effects of high eccentricities on the GWB spectrum.","lang":"eng"}],"status":"public","issue":"3","publication":"Monthly Notices of the Royal Astronomical Society","publisher":"Oxford University Press","author":[{"last_name":"Ryu","full_name":"Ryu, Taeho","first_name":"Taeho"},{"first_name":"Rosalba","last_name":"Perna","full_name":"Perna, Rosalba"},{"first_name":"Zoltán","id":"7c006e8c-cc0d-11ee-8322-cb904ef76f36","full_name":"Haiman, Zoltán","last_name":"Haiman"},{"first_name":"Jeremiah P.","full_name":"Ostriker, Jeremiah P.","last_name":"Ostriker"},{"last_name":"Stone","full_name":"Stone, Nicholas C.","first_name":"Nicholas C."}],"type":"journal_article","date_updated":"2024-09-24T11:14:57Z","day":"27","arxiv":1,"external_id":{"arxiv":["1709.06501"]},"year":"2017","intvolume":"       473","month":"09","publication_status":"published","oa":1,"scopus_import":"1","article_type":"original","citation":{"ama":"Ryu T, Perna R, Haiman Z, Ostriker JP, Stone NC. Interactions between multiple supermassive black holes in galactic nuclei: A solution to the final parsec problem. <i>Monthly Notices of the Royal Astronomical Society</i>. 2017;473(3):3410-3433. doi:<a href=\"https://doi.org/10.1093/mnras/stx2524\">10.1093/mnras/stx2524</a>","apa":"Ryu, T., Perna, R., Haiman, Z., Ostriker, J. P., &#38; Stone, N. C. (2017). Interactions between multiple supermassive black holes in galactic nuclei: A solution to the final parsec problem. <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press. <a href=\"https://doi.org/10.1093/mnras/stx2524\">https://doi.org/10.1093/mnras/stx2524</a>","short":"T. Ryu, R. Perna, Z. Haiman, J.P. Ostriker, N.C. Stone, Monthly Notices of the Royal Astronomical Society 473 (2017) 3410–3433.","ista":"Ryu T, Perna R, Haiman Z, Ostriker JP, Stone NC. 2017. Interactions between multiple supermassive black holes in galactic nuclei: A solution to the final parsec problem. Monthly Notices of the Royal Astronomical Society. 473(3), 3410–3433.","mla":"Ryu, Taeho, et al. “Interactions between Multiple Supermassive Black Holes in Galactic Nuclei: A Solution to the Final Parsec Problem.” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 473, no. 3, Oxford University Press, 2017, pp. 3410–33, doi:<a href=\"https://doi.org/10.1093/mnras/stx2524\">10.1093/mnras/stx2524</a>.","ieee":"T. Ryu, R. Perna, Z. Haiman, J. P. Ostriker, and N. C. Stone, “Interactions between multiple supermassive black holes in galactic nuclei: A solution to the final parsec problem,” <i>Monthly Notices of the Royal Astronomical Society</i>, vol. 473, no. 3. Oxford University Press, pp. 3410–3433, 2017.","chicago":"Ryu, Taeho, Rosalba Perna, Zoltán Haiman, Jeremiah P. Ostriker, and Nicholas C. Stone. “Interactions between Multiple Supermassive Black Holes in Galactic Nuclei: A Solution to the Final Parsec Problem.” <i>Monthly Notices of the Royal Astronomical Society</i>. Oxford University Press, 2017. <a href=\"https://doi.org/10.1093/mnras/stx2524\">https://doi.org/10.1093/mnras/stx2524</a>."},"date_created":"2024-09-05T14:16:56Z","main_file_link":[{"open_access":"1","url":" https://doi.org/10.48550/arXiv.1709.06501"}],"extern":"1","title":"Interactions between multiple supermassive black holes in galactic nuclei: A solution to the final parsec problem","quality_controlled":"1","_id":"17633","user_id":"317138e5-6ab7-11ef-aa6d-ffef3953e345","publication_identifier":{"issn":["0035-8711","1365-2966"]}}]