--- _id: '17731' abstract: - lang: eng text: In cosmological structure formation models, massive non-linear objects in the process of formation, such as galaxy clusters, are surrounded by large-scale shocks at or around the expected virial radius. Direct observational evidence for such virial shocks is currently lacking, but we show here that their presence can be inferred from future, high resolution, high-sensitivity observations of the Sunyaev-Zel'dovich (SZ) effect in galaxy clusters. We study the detectability of virial shocks in mock SZ maps, using simple models of cluster structure (gas density and temperature distributions) and noise (background and foreground galaxy clusters projected along the line of sight, as well as the cosmic microwave background anisotropies). We find that at an angular resolution of 2'' and sensitivity of 10 micro K, expected to be reached at ~ 100 GHz frequencies in a ~ 20 hr integration with the forthcoming ALMA instrument, virial shocks associated with massive M ~ 10^15 M_Sun clusters will stand out from the noise, and can be detected at high significance. More generally, our results imply that the projected SZ surface brightness profile in future, high-resolution experiments will provide sensitive constraints on the density profile of cluster gas. article_processing_charge: No article_type: original author: - first_name: Bence full_name: Kocsis, Bence last_name: Kocsis - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Zsolt full_name: Frei, Zsolt last_name: Frei citation: ama: Kocsis B, Haiman Z, Frei Z. Can virialization shocks be detected around galaxy clusters through the Sunyaev‐Zel’dovich effect? The Astrophysical Journal. 2005;623(2):632-649. doi:10.1086/427975 apa: Kocsis, B., Haiman, Z., & Frei, Z. (2005). Can virialization shocks be detected around galaxy clusters through the Sunyaev‐Zel’dovich effect? The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/427975 chicago: Kocsis, Bence, Zoltán Haiman, and Zsolt Frei. “Can Virialization Shocks Be Detected around Galaxy Clusters through the Sunyaev‐Zel’dovich Effect?” The Astrophysical Journal. American Astronomical Society, 2005. https://doi.org/10.1086/427975. ieee: B. Kocsis, Z. Haiman, and Z. Frei, “Can virialization shocks be detected around galaxy clusters through the Sunyaev‐Zel’dovich effect?,” The Astrophysical Journal, vol. 623, no. 2. American Astronomical Society, pp. 632–649, 2005. ista: Kocsis B, Haiman Z, Frei Z. 2005. Can virialization shocks be detected around galaxy clusters through the Sunyaev‐Zel’dovich effect? The Astrophysical Journal. 623(2), 632–649. mla: Kocsis, Bence, et al. “Can Virialization Shocks Be Detected around Galaxy Clusters through the Sunyaev‐Zel’dovich Effect?” The Astrophysical Journal, vol. 623, no. 2, American Astronomical Society, 2005, pp. 632–49, doi:10.1086/427975. short: B. Kocsis, Z. Haiman, Z. Frei, The Astrophysical Journal 623 (2005) 632–649. date_created: 2024-09-06T09:16:44Z date_published: 2005-04-20T00:00:00Z date_updated: 2024-09-26T07:37:23Z day: '20' doi: 10.1086/427975 extern: '1' intvolume: ' 623' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/427975 month: '04' oa: 1 oa_version: Published Version page: 632-649 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Can virialization shocks be detected around galaxy clusters through the Sunyaev‐Zel’dovich effect? type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 623 year: '2005' ... --- _id: '17737' abstract: - lang: eng text: Cosmological models that include suppression of the power spectrum of density fluctuations on small scales exhibit an exponential reduction of high-redshift, non-linear structures, including a reduction in the rate of gamma ray bursts (GRBs). Here we quantify the constraints that the detection of distant GRBs would place on structure formation models with reduced small-scale power. We compute the number of GRBs that could be detectable by the Swift satellite at high redshifts (z > 6), assuming that the GRBs trace the cosmic star formation history, which itself traces the formation of non-linear structures. We calibrate simple models of the intrinsic luminosity function of the bursts to the number and flux distribution of GRBs observed by the Burst And Transient Source Experiment (BATSE). We find that a discovery of high-z GRBs would imply strong constraints on models with reduced small-scale power. For example, a single GRB at z > 10, or 10 GRBs at z > 5, discovered by Swift during its scheduled two-year mission, would rule out an exponential suppression of the power spectrum on scales below R_c=0.09 Mpc (exemplified by warm dark matter models with a particle mass of m_x=2 keV). Models with a less sharp suppression of small-scale power, such as those with a red tilt or a running scalar index, n_s, are more difficult to constrain, because they are more degenerate with an increase in the power spectrum normalization, sigma_8, and with models in which star-formation is allowed in low-mass minihalos. We find that a tilt of \delta n_s ~ 0.1 is difficult to detect; however, an observed rate of 1 GRB/yr at z > 12 would yield an upper limit on the running of the spectral index, alpha = d(n_s)/d(ln k) > -0.05. article_processing_charge: No article_type: original author: - first_name: Andrei full_name: Mesinger, Andrei last_name: Mesinger - first_name: Rosalba full_name: Perna, Rosalba last_name: Perna - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman citation: ama: Mesinger A, Perna R, Haiman Z. Constraints on the small‐scale power spectrum of density fluctuations from high‐redshift gamma‐ray bursts. The Astrophysical Journal. 2005;623(1):1-10. doi:10.1086/428770 apa: Mesinger, A., Perna, R., & Haiman, Z. (2005). Constraints on the small‐scale power spectrum of density fluctuations from high‐redshift gamma‐ray bursts. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/428770 chicago: Mesinger, Andrei, Rosalba Perna, and Zoltán Haiman. “Constraints on the Small‐scale Power Spectrum of Density Fluctuations from High‐redshift Gamma‐ray Bursts.” The Astrophysical Journal. American Astronomical Society, 2005. https://doi.org/10.1086/428770. ieee: A. Mesinger, R. Perna, and Z. Haiman, “Constraints on the small‐scale power spectrum of density fluctuations from high‐redshift gamma‐ray bursts,” The Astrophysical Journal, vol. 623, no. 1. American Astronomical Society, pp. 1–10, 2005. ista: Mesinger A, Perna R, Haiman Z. 2005. Constraints on the small‐scale power spectrum of density fluctuations from high‐redshift gamma‐ray bursts. The Astrophysical Journal. 623(1), 1–10. mla: Mesinger, Andrei, et al. “Constraints on the Small‐scale Power Spectrum of Density Fluctuations from High‐redshift Gamma‐ray Bursts.” The Astrophysical Journal, vol. 623, no. 1, American Astronomical Society, 2005, pp. 1–10, doi:10.1086/428770. short: A. Mesinger, R. Perna, Z. Haiman, The Astrophysical Journal 623 (2005) 1–10. date_created: 2024-09-06T09:20:42Z date_published: 2005-04-10T00:00:00Z date_updated: 2024-09-26T14:02:13Z day: '10' doi: 10.1086/428770 extern: '1' intvolume: ' 623' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/428770 month: '04' oa: 1 oa_version: Published Version page: 1-10 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Constraints on the small‐scale power spectrum of density fluctuations from high‐redshift gamma‐ray bursts type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 623 year: '2005' ... --- _id: '17761' abstract: - lang: eng text: We explore the possibility of resolving an image of a damped Lyα (DLA) system in absorption against an extended, diffuse, background X-ray source. Typical columns of neutral hydrogen in DLA systems are high enough to block out up to ~30% of the soft X-ray flux at an observed photon energy of 0.5 keV, and we find that ~1% of the area of extended X-ray sources at z ≳ 1 have their 0.5 keV flux reduced by at least 20% because of intervening DLA systems. We discuss the observability of such absorption and find that ≳300 photons per angular resolution element are required in the 0.3-8 keV band for its detection and in order to distinguish it from intrinsic surface brightness fluctuations. For the surface brightness of the currently known high-redshift extended X-ray sources, this requires an integration time of a few megaseconds on Chandra, if the maps are smoothed spatially to ≈2'' resolution. The exact required integration time depends on the DLA system's column density, metallicity, and, most strongly, its redshift. Current X-ray telescopes are likely to detect DLA systems with N < 10^22 cm^-2 only out to z ≈ 2.3. The availability of DLA systems with a suitably high column density for a silhouette detection is currently poorly known. We suggest that at low redshifts archival data of bright X-ray point sources may be useful in constraining the high-N end of the column density distribution. We briefly discuss an alternative strategy of searching for extended X-ray sources behind known DLA systems. Although with current X-ray telescopes the detections are challenging, they will be within the reach of a routine observation with a next generation X-ray telescope, such as the X-Ray Evolving Universe Spectrometer (XEUS) or Generation-X, and will deliver novel constraints on the nature of protogalaxies. article_processing_charge: No article_type: original author: - first_name: Mark full_name: Dijkstra, Mark last_name: Dijkstra - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Caleb full_name: Scharf, Caleb last_name: Scharf citation: ama: Dijkstra M, Haiman Z, Scharf C. On detecting the X‐ray silhouette of a damped Lyα system. The Astrophysical Journal. 2005;624(1):85-93. doi:10.1086/428766 apa: Dijkstra, M., Haiman, Z., & Scharf, C. (2005). On detecting the X‐ray silhouette of a damped Lyα system. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/428766 chicago: Dijkstra, Mark, Zoltán Haiman, and Caleb Scharf. “On Detecting the X‐ray Silhouette of a Damped Lyα System.” The Astrophysical Journal. American Astronomical Society, 2005. https://doi.org/10.1086/428766. ieee: M. Dijkstra, Z. Haiman, and C. Scharf, “On detecting the X‐ray silhouette of a damped Lyα system,” The Astrophysical Journal, vol. 624, no. 1. American Astronomical Society, pp. 85–93, 2005. ista: Dijkstra M, Haiman Z, Scharf C. 2005. On detecting the X‐ray silhouette of a damped Lyα system. The Astrophysical Journal. 624(1), 85–93. mla: Dijkstra, Mark, et al. “On Detecting the X‐ray Silhouette of a Damped Lyα System.” The Astrophysical Journal, vol. 624, no. 1, American Astronomical Society, 2005, pp. 85–93, doi:10.1086/428766. short: M. Dijkstra, Z. Haiman, C. Scharf, The Astrophysical Journal 624 (2005) 85–93. date_created: 2024-09-06T09:48:59Z date_published: 2005-05-01T00:00:00Z date_updated: 2024-09-30T08:55:54Z day: '01' doi: 10.1086/428766 extern: '1' intvolume: ' 624' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/428766 month: '05' oa: 1 oa_version: Published Version page: 85-93 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: On detecting the X‐ray silhouette of a damped Lyα system type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 624 year: '2005' ... --- _id: '17774' abstract: - lang: eng text: We present grism spectra taken with the Advanced Camera for Surveys (ACS) to identify 29 red sources with (i775 - z850) ≥ 0.9 in the Hubble Ultra Deep Field (HUDF). Of these, 23 are found to be galaxies at redshifts between z = 5.4 and 6.7, identified by the break at 1216 Å due to intergalactic medium (IGM) absorption; two are late-type dwarf stars with red colors; and four are galaxies with colors and spectral shapes similar to dust-reddened or old galaxies at redshifts z ≈ 1-2. This constitutes the largest uniform, flux-limited sample of spectroscopically confirmed galaxies at such faint fluxes (z850 ≤ 27.5). Many are also among the most distant spectroscopically confirmed galaxies (at redshifts up to z = 6.7). We find a significant overdensity of galaxies at redshifts z = 5.9 ± 0.2. Nearly two-thirds of the galaxies in our sample (15/23) belong to this peak. Taking into account the selection function and the redshift sensitivity of the survey, we get a conservative overdensity of at least a factor of 2 along the line of sight. The galaxies found in this redshift peak are also localized in the plane of the sky in a nonrandom manner, occupying about half of the ACS chip. Thus the volume overdensity is a factor of 4. The star formation rate derived from detected sources in this overdense region is sufficient to reionize the local IGM. article_processing_charge: No article_type: original author: - first_name: S. full_name: Malhotra, S. last_name: Malhotra - first_name: J. E. full_name: Rhoads, J. E. last_name: Rhoads - first_name: N. full_name: Pirzkal, N. last_name: Pirzkal - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: C. full_name: Xu, C. last_name: Xu - first_name: E. full_name: Daddi, E. last_name: Daddi - first_name: H. full_name: Yan, H. last_name: Yan - first_name: L. E. full_name: Bergeron, L. E. last_name: Bergeron - first_name: J. full_name: Wang, J. last_name: Wang - first_name: H. C. full_name: Ferguson, H. C. last_name: Ferguson - first_name: C. full_name: Gronwall, C. last_name: Gronwall - first_name: A. full_name: Koekemoer, A. last_name: Koekemoer - first_name: M. full_name: Kuemmel, M. last_name: Kuemmel - first_name: L. A. full_name: Moustakas, L. A. last_name: Moustakas - first_name: N. full_name: Panagia, N. last_name: Panagia - first_name: A. full_name: Pasquali, A. last_name: Pasquali - first_name: M. full_name: Stiavelli, M. last_name: Stiavelli - first_name: J. full_name: Walsh, J. last_name: Walsh - first_name: R. A. full_name: Windhorst, R. A. last_name: Windhorst - first_name: S. full_name: di Serego Alighieri, S. last_name: di Serego Alighieri citation: ama: Malhotra S, Rhoads JE, Pirzkal N, et al. An overdensity of galaxies at z= 5.9 ± 0.2 in the Hubble Ultra Deep Field confirmed using the ACS grism. The Astrophysical Journal. 2005;626(2):666-679. doi:10.1086/430047 apa: Malhotra, S., Rhoads, J. E., Pirzkal, N., Haiman, Z., Xu, C., Daddi, E., … di Serego Alighieri, S. (2005). An overdensity of galaxies at z= 5.9 ± 0.2 in the Hubble Ultra Deep Field confirmed using the ACS grism. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/430047 chicago: Malhotra, S., J. E. Rhoads, N. Pirzkal, Zoltán Haiman, C. Xu, E. Daddi, H. Yan, et al. “An Overdensity of Galaxies at Z= 5.9 ± 0.2 in the Hubble Ultra Deep Field Confirmed Using the ACS Grism.” The Astrophysical Journal. American Astronomical Society, 2005. https://doi.org/10.1086/430047. ieee: S. Malhotra et al., “An overdensity of galaxies at z= 5.9 ± 0.2 in the Hubble Ultra Deep Field confirmed using the ACS grism,” The Astrophysical Journal, vol. 626, no. 2. American Astronomical Society, pp. 666–679, 2005. ista: Malhotra S, Rhoads JE, Pirzkal N, Haiman Z, Xu C, Daddi E, Yan H, Bergeron LE, Wang J, Ferguson HC, Gronwall C, Koekemoer A, Kuemmel M, Moustakas LA, Panagia N, Pasquali A, Stiavelli M, Walsh J, Windhorst RA, di Serego Alighieri S. 2005. An overdensity of galaxies at z= 5.9 ± 0.2 in the Hubble Ultra Deep Field confirmed using the ACS grism. The Astrophysical Journal. 626(2), 666–679. mla: Malhotra, S., et al. “An Overdensity of Galaxies at Z= 5.9 ± 0.2 in the Hubble Ultra Deep Field Confirmed Using the ACS Grism.” The Astrophysical Journal, vol. 626, no. 2, American Astronomical Society, 2005, pp. 666–79, doi:10.1086/430047. short: S. Malhotra, J.E. Rhoads, N. Pirzkal, Z. Haiman, C. Xu, E. Daddi, H. Yan, L.E. Bergeron, J. Wang, H.C. Ferguson, C. Gronwall, A. Koekemoer, M. Kuemmel, L.A. Moustakas, N. Panagia, A. Pasquali, M. Stiavelli, J. Walsh, R.A. Windhorst, S. di Serego Alighieri, The Astrophysical Journal 626 (2005) 666–679. date_created: 2024-09-06T10:04:19Z date_published: 2005-06-20T00:00:00Z date_updated: 2024-09-30T11:34:11Z day: '20' doi: 10.1086/430047 extern: '1' intvolume: ' 626' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/430047 month: '06' oa: 1 oa_version: Published Version page: 666-679 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: An overdensity of galaxies at z= 5.9 ± 0.2 in the Hubble Ultra Deep Field confirmed using the ACS grism type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 626 year: '2005' ... --- _id: '17781' abstract: - lang: eng text: We have discovered an extended Lyα plume (UDF 5225) associated with a compact source at redshift z ≈ 5.4 in slitless spectroscopic data from the Grism ACS Program for Extragalactic Science (GRAPES) project. The spatial extent of the emission is about 6 × 1.5 kpc (1'' × 0farcs25). Combining our grism data and the broadband images from the Hubble Ultra Deep Field (UDF) images, we find a Lyα line flux of ~2.2 × 10^-17 ergs cm^-2 s^-1 and surface brightness ~7 × 10^-17ergs cm^-2 s-1 arcsec^-2. The UDF images show diffuse continuum emission associated with UDF 5225, including three embedded knots. The morphology of UDF 5225 is highly suggestive of a galaxy in assembly. It is possible that the prominent Lyα emission from this object is due to an active nucleus, and that we are seeing the simultaneous growth through accretion of a galaxy and its central black hole. Follow-up observations at higher spectral resolution could test this hypothesis. article_processing_charge: No article_type: original author: - first_name: James E. full_name: Rhoads, James E. last_name: Rhoads - first_name: Nino full_name: Panagia, Nino last_name: Panagia - first_name: Rogier A. full_name: Windhorst, Rogier A. last_name: Windhorst - first_name: Sangeeta full_name: Malhotra, Sangeeta last_name: Malhotra - first_name: Norbert full_name: Pirzkal, Norbert last_name: Pirzkal - first_name: Chun full_name: Xu, Chun last_name: Xu - first_name: Louis Gregory full_name: Strolger, Louis Gregory last_name: Strolger - first_name: Louis E. full_name: Bergeron, Louis E. last_name: Bergeron - first_name: Emanuele full_name: Daddi, Emanuele last_name: Daddi - first_name: Harry full_name: Ferguson, Harry last_name: Ferguson - first_name: Jonathan P. full_name: Gardner, Jonathan P. last_name: Gardner - first_name: Caryl full_name: Gronwall, Caryl last_name: Gronwall - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Anton full_name: Koekemoer, Anton last_name: Koekemoer - first_name: Martin full_name: Kummel, Martin last_name: Kummel - first_name: Leonidas A. full_name: Moustakas, Leonidas A. last_name: Moustakas - first_name: Anna full_name: Pasquali, Anna last_name: Pasquali - first_name: Adam full_name: Riess, Adam last_name: Riess - first_name: Sperello full_name: di Serego Alighieri, Sperello last_name: di Serego Alighieri - first_name: Massimo full_name: Stiavelli, Massimo last_name: Stiavelli - first_name: Zlatan full_name: Tsvetanov, Zlatan last_name: Tsvetanov - first_name: Joel full_name: Vernet, Joel last_name: Vernet - first_name: Jeremy full_name: Walsh, Jeremy last_name: Walsh - first_name: Haojing full_name: Yan, Haojing last_name: Yan citation: ama: Rhoads JE, Panagia N, Windhorst RA, et al. A redshift z≈ 5.4 Lyα emitting galaxy with linear morphology in the GRAPES/Hubble Ultra Deep Field. The Astrophysical Journal. 2005;621(2):582-586. doi:10.1086/427622 apa: Rhoads, J. E., Panagia, N., Windhorst, R. A., Malhotra, S., Pirzkal, N., Xu, C., … Yan, H. (2005). A redshift z≈ 5.4 Lyα emitting galaxy with linear morphology in the GRAPES/Hubble Ultra Deep Field. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/427622 chicago: Rhoads, James E., Nino Panagia, Rogier A. Windhorst, Sangeeta Malhotra, Norbert Pirzkal, Chun Xu, Louis Gregory Strolger, et al. “A Redshift Z≈ 5.4 Lyα Emitting Galaxy with Linear Morphology in the GRAPES/Hubble Ultra Deep Field.” The Astrophysical Journal. American Astronomical Society, 2005. https://doi.org/10.1086/427622. ieee: J. E. Rhoads et al., “A redshift z≈ 5.4 Lyα emitting galaxy with linear morphology in the GRAPES/Hubble Ultra Deep Field,” The Astrophysical Journal, vol. 621, no. 2. American Astronomical Society, pp. 582–586, 2005. ista: Rhoads JE, Panagia N, Windhorst RA, Malhotra S, Pirzkal N, Xu C, Strolger LG, Bergeron LE, Daddi E, Ferguson H, Gardner JP, Gronwall C, Haiman Z, Koekemoer A, Kummel M, Moustakas LA, Pasquali A, Riess A, di Serego Alighieri S, Stiavelli M, Tsvetanov Z, Vernet J, Walsh J, Yan H. 2005. A redshift z≈ 5.4 Lyα emitting galaxy with linear morphology in the GRAPES/Hubble Ultra Deep Field. The Astrophysical Journal. 621(2), 582–586. mla: Rhoads, James E., et al. “A Redshift Z≈ 5.4 Lyα Emitting Galaxy with Linear Morphology in the GRAPES/Hubble Ultra Deep Field.” The Astrophysical Journal, vol. 621, no. 2, American Astronomical Society, 2005, pp. 582–86, doi:10.1086/427622. short: J.E. Rhoads, N. Panagia, R.A. Windhorst, S. Malhotra, N. Pirzkal, C. Xu, L.G. Strolger, L.E. Bergeron, E. Daddi, H. Ferguson, J.P. Gardner, C. Gronwall, Z. Haiman, A. Koekemoer, M. Kummel, L.A. Moustakas, A. Pasquali, A. Riess, S. di Serego Alighieri, M. Stiavelli, Z. Tsvetanov, J. Vernet, J. Walsh, H. Yan, The Astrophysical Journal 621 (2005) 582–586. date_created: 2024-09-06T10:15:40Z date_published: 2005-05-10T00:00:00Z date_updated: 2024-09-30T12:17:32Z day: '10' doi: 10.1086/427622 extern: '1' intvolume: ' 621' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/427622 month: '05' oa: 1 oa_version: Published Version page: 582-586 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: A redshift z≈ 5.4 Lyα emitting galaxy with linear morphology in the GRAPES/Hubble Ultra Deep Field type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 621 year: '2005' ... --- _id: '17717' abstract: - lang: eng text: We demonstrate that constraints on cosmological parameters from the distribution of clusters as a function of redshift (dN/dz) are complementary to accurate angular diameter distance (D_A) measurements to clusters, and their combination significantly tightens constraints on the energy density content of the Universe. The number counts can be obtained from X-ray and/or SZ (Sunyaev-Zel'dovich effect) surveys, and the angular diameter distances can be determined from deep observations of the intra-cluster gas using their thermal bremsstrahlung X-ray emission and the SZ effect. We combine constraints from simulated cluster number counts expected from a 12 deg^2 SZ cluster survey and constraints from simulated angular diameter distance measurements based on the X-ray/SZ method assuming a statistical accuracy of 10% in the angular diameter distance determination of 100 clusters with redshifts less than 1.5. We find that Omega_m can be determined within about 25%, Omega_Lambda within 20%, and w within 16%. We show that combined dN/dz + D_A constraints can be used to constrain the different energy densities in the Universe even in the presence of a few percent redshift dependent systematic error in D_A. We also address the question of how best to select clusters of galaxies for accurate diameter distance determinations. We show that the joint dN/dz + D_A constraints on cosmological parameters for a fixed target accuracy in the energy density parameters are optimized by selecting clusters with redshift upper cut--offs in the range 0.5 < z < 1. article_processing_charge: No article_type: original author: - first_name: Sandor M. full_name: Molnar, Sandor M. last_name: Molnar - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Mark full_name: Birkinshaw, Mark last_name: Birkinshaw - first_name: Richard F. full_name: Mushotzky, Richard F. last_name: Mushotzky citation: ama: Molnar SM, Haiman Z, Birkinshaw M, Mushotzky RF. Constraints on the energy content of the universe from a combination of galaxy cluster observables. The Astrophysical Journal. 2004;601(1):22-27. doi:10.1086/380295 apa: Molnar, S. M., Haiman, Z., Birkinshaw, M., & Mushotzky, R. F. (2004). Constraints on the energy content of the universe from a combination of galaxy cluster observables. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/380295 chicago: Molnar, Sandor M., Zoltán Haiman, Mark Birkinshaw, and Richard F. Mushotzky. “Constraints on the Energy Content of the Universe from a Combination of Galaxy Cluster Observables.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/380295. ieee: S. M. Molnar, Z. Haiman, M. Birkinshaw, and R. F. Mushotzky, “Constraints on the energy content of the universe from a combination of galaxy cluster observables,” The Astrophysical Journal, vol. 601, no. 1. American Astronomical Society, pp. 22–27, 2004. ista: Molnar SM, Haiman Z, Birkinshaw M, Mushotzky RF. 2004. Constraints on the energy content of the universe from a combination of galaxy cluster observables. The Astrophysical Journal. 601(1), 22–27. mla: Molnar, Sandor M., et al. “Constraints on the Energy Content of the Universe from a Combination of Galaxy Cluster Observables.” The Astrophysical Journal, vol. 601, no. 1, American Astronomical Society, 2004, pp. 22–27, doi:10.1086/380295. short: S.M. Molnar, Z. Haiman, M. Birkinshaw, R.F. Mushotzky, The Astrophysical Journal 601 (2004) 22–27. date_created: 2024-09-06T09:02:16Z date_published: 2004-01-20T00:00:00Z date_updated: 2024-09-25T13:08:12Z day: '20' doi: 10.1086/380295 extern: '1' intvolume: ' 601' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/380295 month: '01' oa: 1 oa_version: Published Version page: 22-27 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Constraints on the energy content of the universe from a combination of galaxy cluster observables type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 601 year: '2004' ... --- _id: '17725' abstract: - lang: eng text: A bright quasar residing in a dense and largely neutral intergalactic medium (IGM) at high redshifts (z > 6) will be surrounded by a large cosmological Stromgren sphere. The quasar's spectrum will then show a sharp increase in resonant Lyman line absorption at wavelengths approaching and shorter than that corresponding to the Stromgren sphere's boundary along the line of sight. We show here that simultaneously considering the measured absorption in two or more hydrogen Lyman lines can provide the dynamical range required to detect this feature. We model broad and robust features of the Lyman alpha and Lyman beta regions of the spectrum of the z=6.28 quasar SDSS J1030+0524, using a hydrodynamical simulation. From the steep wavelength-dependence of the inferred absorption opacity, we detect the boundary of the Stromgren sphere at a proper distance of 6.0 +/- 0.2 Mpc away from the source redshift. From the spectrum alone, we also find that beyond this distance, cosmic hydrogen turns nearly neutral, with a neutral fraction of x_HI > 0.2, and that the ionizing luminosity of this quasar is in the range (5.2 +/- 2.5) times 10^{56} photons/sec. The method presented here, when applied to future quasars, can probe the complex topology of overlapping ionized regions, and can be used to study the details of the reionization process. article_processing_charge: No article_type: original author: - first_name: Andrei full_name: Mesinger, Andrei last_name: Mesinger - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman citation: ama: Mesinger A, Haiman Z. Evidence of a cosmological Strömgren surface and of significant neutral hydrogen surrounding the quasar SDSS J1030+0524. The Astrophysical Journal. 2004;611(2):L69-L72. doi:10.1086/423935 apa: Mesinger, A., & Haiman, Z. (2004). Evidence of a cosmological Strömgren surface and of significant neutral hydrogen surrounding the quasar SDSS J1030+0524. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/423935 chicago: Mesinger, Andrei, and Zoltán Haiman. “Evidence of a Cosmological Strömgren Surface and of Significant Neutral Hydrogen Surrounding the Quasar SDSS J1030+0524.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/423935. ieee: A. Mesinger and Z. Haiman, “Evidence of a cosmological Strömgren surface and of significant neutral hydrogen surrounding the quasar SDSS J1030+0524,” The Astrophysical Journal, vol. 611, no. 2. American Astronomical Society, pp. L69–L72, 2004. ista: Mesinger A, Haiman Z. 2004. Evidence of a cosmological Strömgren surface and of significant neutral hydrogen surrounding the quasar SDSS J1030+0524. The Astrophysical Journal. 611(2), L69–L72. mla: Mesinger, Andrei, and Zoltán Haiman. “Evidence of a Cosmological Strömgren Surface and of Significant Neutral Hydrogen Surrounding the Quasar SDSS J1030+0524.” The Astrophysical Journal, vol. 611, no. 2, American Astronomical Society, 2004, pp. L69–72, doi:10.1086/423935. short: A. Mesinger, Z. Haiman, The Astrophysical Journal 611 (2004) L69–L72. date_created: 2024-09-06T09:12:22Z date_published: 2004-07-19T00:00:00Z date_updated: 2024-09-25T14:12:20Z day: '19' doi: 10.1086/423935 extern: '1' intvolume: ' 611' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/423935 month: '07' oa: 1 oa_version: Published Version page: L69-L72 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Evidence of a cosmological Strömgren surface and of significant neutral hydrogen surrounding the quasar SDSS J1030+0524 type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 611 year: '2004' ... --- _id: '17728' abstract: - lang: eng text: The cosmic ultraviolet (UV) ionizing background impacts the formation of dwarf galaxies in the low-redshift universe (z=3) by suppressing gas infall into galactic halos with circular velocities up to v(circ)=75 km/s. Using a one-dimensional, spherically symmetric hydrodynamics code (Thoul & Weinberg 1995), we examine the effect of an ionizing background on low-mass galaxies forming at high redshifts (z>10). We find that the importance of photoionization feedback is greatly reduced, because (1) at high redshift, dwarf-galaxy sized objects can self-shield against the ionizing background, (2) collisional cooling processes at high redshift are more efficient, (3) the amplitude of the ionizing background at high redshift is lower, and (4) the ionizing radiation turns on when the perturbation that will become the dwarf galaxy has already grown to a substantial overdensity. We find that because of these reasons, gas can collect inside halos with circular velocities as low as v(circ)=10 km/s. This result has important implications for the reionization history of the universe. article_processing_charge: No article_type: original author: - first_name: Mark full_name: Dijkstra, Mark last_name: Dijkstra - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Martin J. full_name: Rees, Martin J. last_name: Rees - first_name: David H. full_name: Weinberg, David H. last_name: Weinberg citation: ama: Dijkstra M, Haiman Z, Rees MJ, Weinberg DH. Photoionization feedback in low‐mass galaxies at high redshift. The Astrophysical Journal. 2004;601(2):666-675. doi:10.1086/380603 apa: Dijkstra, M., Haiman, Z., Rees, M. J., & Weinberg, D. H. (2004). Photoionization feedback in low‐mass galaxies at high redshift. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/380603 chicago: Dijkstra, Mark, Zoltán Haiman, Martin J. Rees, and David H. Weinberg. “Photoionization Feedback in Low‐mass Galaxies at High Redshift.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/380603. ieee: M. Dijkstra, Z. Haiman, M. J. Rees, and D. H. Weinberg, “Photoionization feedback in low‐mass galaxies at high redshift,” The Astrophysical Journal, vol. 601, no. 2. American Astronomical Society, pp. 666–675, 2004. ista: Dijkstra M, Haiman Z, Rees MJ, Weinberg DH. 2004. Photoionization feedback in low‐mass galaxies at high redshift. The Astrophysical Journal. 601(2), 666–675. mla: Dijkstra, Mark, et al. “Photoionization Feedback in Low‐mass Galaxies at High Redshift.” The Astrophysical Journal, vol. 601, no. 2, American Astronomical Society, 2004, pp. 666–75, doi:10.1086/380603. short: M. Dijkstra, Z. Haiman, M.J. Rees, D.H. Weinberg, The Astrophysical Journal 601 (2004) 666–675. date_created: 2024-09-06T09:14:46Z date_published: 2004-02-01T00:00:00Z date_updated: 2024-09-26T07:26:27Z day: '01' doi: 10.1086/380603 extern: '1' intvolume: ' 601' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/380603 month: '02' oa: 1 oa_version: Published Version page: 666-675 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Photoionization feedback in low‐mass galaxies at high redshift type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 601 year: '2004' ... --- _id: '17743' abstract: - lang: eng text: We use a physically motivated semi-analytic model, based on the mass function of dark matter halos, to predict the number of radio-loud quasars as a function of redshift and luminosity. Simple models in which the central BH mass scales with the velocity dispersion of its host halo as M(bh) sigma(halo)^5 have been previously found to be consistent with a number of observations, including the optical and X-ray quasar luminosity functions. We find that similar models, when augmented with an empirical prescription for radio emission, overpredict the number of faint (10 micro-Jy) radio sources by 1-2 orders of magnitude. This translates into a more stringent constraint on the low-mass end of the quasar black hole mass function than is available from the Hubble and Chandra Deep Fields. We interpret this discrepancy as evidence that black holes with masses below 10^7 Msun are either rare or are not as radio-loud as their more massive counterparts. Models that exclude BHs with masses below 10^7 Msun are in agreement with the deepest existing radio observations, but still produce a significant tail of high-redshift objects. In the 1-10GHz bands, at the sensitivity of 10 micro-Jy, we find surface densities of 100, 10, and 0.3 deg^-2 for sources located at z>6, 10, and 15, respectively. The discovery of these sources with instruments such as the Allen Telescope Array (ATA), Extended Very Large Array (EVLA), and the Square Kilometer Array (SKA) would open a new window for the study of supermassive BHs at high redshift. We also find surface densities of 0.1 deg^-2 at z > 6 for mJy sources that can be used to study 21 cm absorption from the epoch of reionization. We suggest that, although not yet optically identified, the FIRST survey may have already detected 10^3-10^4 such sources. article_processing_charge: No article_type: original author: - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Eliot full_name: Quataert, Eliot last_name: Quataert - first_name: Geoffrey C. full_name: Bower, Geoffrey C. last_name: Bower citation: ama: 'Haiman Z, Quataert E, Bower GC. Modeling the counts of faint radio‐loud quasars: Constraints on the supermassive black hole population and predictions for high redshift. The Astrophysical Journal. 2004;612(2):698-705. doi:10.1086/422834' apa: 'Haiman, Z., Quataert, E., & Bower, G. C. (2004). Modeling the counts of faint radio‐loud quasars: Constraints on the supermassive black hole population and predictions for high redshift. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/422834' chicago: 'Haiman, Zoltán, Eliot Quataert, and Geoffrey C. Bower. “Modeling the Counts of Faint Radio‐loud Quasars: Constraints on the Supermassive Black Hole Population and Predictions for High Redshift.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/422834.' ieee: 'Z. Haiman, E. Quataert, and G. C. Bower, “Modeling the counts of faint radio‐loud quasars: Constraints on the supermassive black hole population and predictions for high redshift,” The Astrophysical Journal, vol. 612, no. 2. American Astronomical Society, pp. 698–705, 2004.' ista: 'Haiman Z, Quataert E, Bower GC. 2004. Modeling the counts of faint radio‐loud quasars: Constraints on the supermassive black hole population and predictions for high redshift. The Astrophysical Journal. 612(2), 698–705.' mla: 'Haiman, Zoltán, et al. “Modeling the Counts of Faint Radio‐loud Quasars: Constraints on the Supermassive Black Hole Population and Predictions for High Redshift.” The Astrophysical Journal, vol. 612, no. 2, American Astronomical Society, 2004, pp. 698–705, doi:10.1086/422834.' short: Z. Haiman, E. Quataert, G.C. Bower, The Astrophysical Journal 612 (2004) 698–705. date_created: 2024-09-06T09:27:01Z date_published: 2004-09-10T00:00:00Z date_updated: 2024-09-26T14:20:17Z day: '10' doi: 10.1086/422834 extern: '1' intvolume: ' 612' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/422834 month: '09' oa: 1 oa_version: Published Version page: 698-705 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: 'Modeling the counts of faint radio‐loud quasars: Constraints on the supermassive black hole population and predictions for high redshift' type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 612 year: '2004' ... --- _id: '17745' abstract: - lang: eng text: We quantify and discuss the footprints of neutral hydrogen in the intergalactic medium (IGM) on the spectra of high-redshift (z ~ 6) sources, using mock spectra generated from hydrodynamical simulations of the IGM. We show that it should be possible to extract relevant parameters, including the mean neutral fraction in the IGM and the radius of the local cosmological Strömgren region, from the flux distribution in the observed spectra of distant sources. We focus on quasars, but a similar analysis is applicable to galaxies and gamma-ray burst (GRB) afterglows. We explicitly include uncertainties in the spectral shape of the assumed source template near the Lyα line. Our results suggest that a mean neutral hydrogen fraction, xH, of unity can be statistically distinguished from xH ≈ 10^-2 by combining the spectra of tens of bright (M ≈ -27) quasars. Alternatively, the same distinction can be achieved using the spectra of several hundred sources that are ~100 times fainter. Furthermore, if the radius of the Strömgren sphere can be independently constrained to within ~10%, this distinction can be achieved using a single source. The information derived from such spectra will help in settling the current debate as to what extent the universe was reionized at redshifts near z ~ 6. article_processing_charge: No article_type: original author: - first_name: Andrei full_name: Mesinger, Andrei last_name: Mesinger - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Renyue full_name: Cen, Renyue last_name: Cen citation: ama: Mesinger A, Haiman Z, Cen R. Probing the reionization history using the spectra of high‐redshift sources. The Astrophysical Journal. 2004;613(1):23-35. doi:10.1086/422898 apa: Mesinger, A., Haiman, Z., & Cen, R. (2004). Probing the reionization history using the spectra of high‐redshift sources. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/422898 chicago: Mesinger, Andrei, Zoltán Haiman, and Renyue Cen. “Probing the Reionization History Using the Spectra of High‐redshift Sources.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/422898. ieee: A. Mesinger, Z. Haiman, and R. Cen, “Probing the reionization history using the spectra of high‐redshift sources,” The Astrophysical Journal, vol. 613, no. 1. American Astronomical Society, pp. 23–35, 2004. ista: Mesinger A, Haiman Z, Cen R. 2004. Probing the reionization history using the spectra of high‐redshift sources. The Astrophysical Journal. 613(1), 23–35. mla: Mesinger, Andrei, et al. “Probing the Reionization History Using the Spectra of High‐redshift Sources.” The Astrophysical Journal, vol. 613, no. 1, American Astronomical Society, 2004, pp. 23–35, doi:10.1086/422898. short: A. Mesinger, Z. Haiman, R. Cen, The Astrophysical Journal 613 (2004) 23–35. date_created: 2024-09-06T09:34:05Z date_published: 2004-09-20T00:00:00Z date_updated: 2024-09-26T14:26:47Z day: '20' doi: 10.1086/422898 extern: '1' intvolume: ' 613' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/422898 month: '09' oa: 1 oa_version: Published Version page: 23-35 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Probing the reionization history using the spectra of high‐redshift sources type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 613 year: '2004' ... --- _id: '17758' abstract: - lang: eng text: Krstic has carried out the first quantum mechanical calculations near threshold for the charge transfer (CT) process H^+ + H_2(X ^1Sigma_g^+, nu=0, J=0) --> H(1s) + H_2^+. These results are relevant for models of primordial galaxy and first star formation that require reliable atomic and molecular data for obtaining the early universe hydrogen chemistry. Using the results of Krstic, we calculate the relevant CT rate coefficient for temperatures between 100 and 30,000 K. We also present a simple fit which can be readily implemented into early universe chemical models. Additionally, we explore how the range of previously published data for this reaction translates into uncertainties in the predicted gas temperature and H_2 relative abundance in a collapsing primordial gas cloud. Our new data significantly reduce these cosmological uncertainties that are due to the uncertainties in the previously published CT rate coefficients. article_processing_charge: No article_type: original author: - first_name: Daniel Wolf full_name: Savin, Daniel Wolf last_name: Savin - first_name: Predrag S. full_name: Krsti, Predrag S. last_name: Krsti - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Phillip C. full_name: Stancil, Phillip C. last_name: Stancil citation: ama: Savin DW, Krsti PS, Haiman Z, Stancil PC. Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications. The Astrophysical Journal. 2004;606(2):L167-L170. doi:10.1086/421108 apa: Savin, D. W., Krsti, P. S., Haiman, Z., & Stancil, P. C. (2004). Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/421108 chicago: Savin, Daniel Wolf, Predrag S. Krsti, Zoltán Haiman, and Phillip C. Stancil. “Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/421108. ieee: D. W. Savin, P. S. Krsti, Z. Haiman, and P. C. Stancil, “Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications,” The Astrophysical Journal, vol. 606, no. 2. American Astronomical Society, pp. L167–L170, 2004. ista: Savin DW, Krsti PS, Haiman Z, Stancil PC. 2004. Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications. The Astrophysical Journal. 606(2), L167–L170. mla: Savin, Daniel Wolf, et al. “Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications.” The Astrophysical Journal, vol. 606, no. 2, American Astronomical Society, 2004, pp. L167–70, doi:10.1086/421108. short: D.W. Savin, P.S. Krsti, Z. Haiman, P.C. Stancil, The Astrophysical Journal 606 (2004) L167–L170. date_created: 2024-09-06T09:45:29Z date_published: 2004-05-10T00:00:00Z date_updated: 2024-09-26T14:12:52Z day: '10' doi: 10.1086/421108 extern: '1' intvolume: ' 606' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/421108 month: '05' oa: 1 oa_version: Published Version page: L167-L170 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' related_material: link: - relation: erratum url: https://doi.org/10.1086/421873 scopus_import: '1' status: public title: Rate Coefficient for H+ + H2(X1Σg+, ν = 0, J = 0) → H(1s) + H2+ Charge Transfer and Some Cosmological Implications type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 606 year: '2004' ... --- _id: '17763' abstract: - lang: eng text: Recent studies have suggested that during their coalescence, binary supermassive black holes (SMBHs) experience typical gravitational recoil velocities that may be as large as ≳100 km s^-1. These velocities exceed the escape velocity vesc from typical dark matter (DM) halos at high redshift (z ≳ 6), and therefore put constraints on scenarios in which early SMBHs grow at the centers of DM halos. Here we quantify these constraints for the most distant known SMBH, with an inferred mass in excess of 10^9 M☉, powering the bright quasar SDSS J1148+5251 discovered in the Sloan Digital Sky Survey at z = 6.43. We assume that this SMBH grew via a combination of accretion and mergers between preexisting seed BHs in individual progenitor halos, and that mergers between progenitors with vesc < vkick disrupt the BH growth process. Our results suggest that under these assumptions, the z ≈ 6 SMBHs had a phase during which they gained mass vary rapidly. In particular, typical z ≈ 3 quasars with luminosities similar to that of SDSS J1148+5251 have recently been inferred to have an average radiative efficiency of epsilon ≈ 20%. The growth rate of the SMBH in SDSS J1148+5251 must have significantly exceeded the Eddington accretion rate with this efficiency. article_processing_charge: No article_type: original author: - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman citation: ama: Haiman Z. Constraints from gravitational recoil on the growth of supermassive black holes at high redshift. The Astrophysical Journal. 2004;613(1):36-40. doi:10.1086/422910 apa: Haiman, Z. (2004). Constraints from gravitational recoil on the growth of supermassive black holes at high redshift. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/422910 chicago: Haiman, Zoltán. “Constraints from Gravitational Recoil on the Growth of Supermassive Black Holes at High Redshift.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/422910. ieee: Z. Haiman, “Constraints from gravitational recoil on the growth of supermassive black holes at high redshift,” The Astrophysical Journal, vol. 613, no. 1. American Astronomical Society, pp. 36–40, 2004. ista: Haiman Z. 2004. Constraints from gravitational recoil on the growth of supermassive black holes at high redshift. The Astrophysical Journal. 613(1), 36–40. mla: Haiman, Zoltán. “Constraints from Gravitational Recoil on the Growth of Supermassive Black Holes at High Redshift.” The Astrophysical Journal, vol. 613, no. 1, American Astronomical Society, 2004, pp. 36–40, doi:10.1086/422910. short: Z. Haiman, The Astrophysical Journal 613 (2004) 36–40. date_created: 2024-09-06T09:50:34Z date_published: 2004-09-20T00:00:00Z date_updated: 2024-09-30T09:12:19Z day: '20' doi: 10.1086/422910 extern: '1' intvolume: ' 613' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/422910 month: '09' oa: 1 oa_version: Published Version page: 36-40 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Constraints from gravitational recoil on the growth of supermassive black holes at high redshift type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 613 year: '2004' ... --- _id: '17775' abstract: - lang: eng text: 'We discuss a simple model for the growth of supermassive black holes (BHs) at the center of spheroidal stellar systems. In particular, we assess the hypotheses that (1) star formation in spheroids and BH fueling are proportional to one another, and (2) the BH accretion luminosity stays near the Eddington limit during luminous quasar phases. With the aid of this simple model, we are able to interpret many properties of the QSO luminosity function, including the puzzling steep decline of the characteristic luminosity from redshift z=2 to to z=0: indeed the residual star formation in spheroidal systems is today limited to a small number of bulges, characterized by stellar velocity dispersions a factor of 2-3 smaller those of the elliptical galaxies hosting QSOs at z > 2. A simple consequence of our hypotheses is that the redshift evolution of the QSO emissivity and of the star formation history in spheroids should be roughly parallel. We find this result to be broadly consistent with our knowledge of the evolution of both the global star formation rate, and of the evolution of the QSO emissivity, but we identify interesting discrepancies at both low and high redshifts, to which we offer tentative solutions. Finally, our hypotheses allow us to present a robust method to derive the duty cycle of QSO activity, based on the observed QSO luminosity function, and on the present-day relation between the masses of supermassive BHs and those of their spheroidal host stellar systems. The duty cycle is found to be substantially less than unity, with characteristic values in the range (3-6)x10^(-3), and we compute that the average bolometric radiative efficiency is epsilon=0.07. Finally, we find that the growth in mass of individual black holes at high redshift (z>2) can be dominated by mergers, and is therefore not necessarily limited by accretion.' article_processing_charge: No article_type: original author: - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Luca full_name: Ciotti, Luca last_name: Ciotti - first_name: Jeremiah P. full_name: Ostriker, Jeremiah P. last_name: Ostriker citation: ama: 'Haiman Z, Ciotti L, Ostriker JP. Reasoning from fossils: Learning from the local black hole population about the evolution of quasars. The Astrophysical Journal. 2004;606(2):763-773. doi:10.1086/383022' apa: 'Haiman, Z., Ciotti, L., & Ostriker, J. P. (2004). Reasoning from fossils: Learning from the local black hole population about the evolution of quasars. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/383022' chicago: 'Haiman, Zoltán, Luca Ciotti, and Jeremiah P. Ostriker. “Reasoning from Fossils: Learning from the Local Black Hole Population about the Evolution of Quasars.” The Astrophysical Journal. American Astronomical Society, 2004. https://doi.org/10.1086/383022.' ieee: 'Z. Haiman, L. Ciotti, and J. P. Ostriker, “Reasoning from fossils: Learning from the local black hole population about the evolution of quasars,” The Astrophysical Journal, vol. 606, no. 2. American Astronomical Society, pp. 763–773, 2004.' ista: 'Haiman Z, Ciotti L, Ostriker JP. 2004. Reasoning from fossils: Learning from the local black hole population about the evolution of quasars. The Astrophysical Journal. 606(2), 763–773.' mla: 'Haiman, Zoltán, et al. “Reasoning from Fossils: Learning from the Local Black Hole Population about the Evolution of Quasars.” The Astrophysical Journal, vol. 606, no. 2, American Astronomical Society, 2004, pp. 763–73, doi:10.1086/383022.' short: Z. Haiman, L. Ciotti, J.P. Ostriker, The Astrophysical Journal 606 (2004) 763–773. date_created: 2024-09-06T10:07:44Z date_published: 2004-05-10T00:00:00Z date_updated: 2024-09-30T11:41:03Z day: '10' doi: 10.1086/383022 extern: '1' intvolume: ' 606' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/383022 month: '05' oa: 1 oa_version: Published Version page: 763-773 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: 'Reasoning from fossils: Learning from the local black hole population about the evolution of quasars' type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 606 year: '2004' ... --- _id: '17741' abstract: - lang: eng text: The recent discovery of a Gunn-Peterson (GP) trough in the spectrum of the redshift 6.28 SDSS quasar has raised the tantalizing possibility that we have detected the reionization of the universe. However, a neutral fraction (of hydrogen) as small as 0.1% is sufficient to cause the GP trough; hence, its detection alone cannot rule out reionization at a much earlier epoch. The cosmic microwave background (CMB) polarization anisotropy offers an alternative way to explore the dark age of the universe. We show that for most models constrained by the current CMB data and by the discovery of a GP trough (showing that reionization occurred at z > 6.3), Microwave Anisotropy Probe (MAP) can detect the reionization signature in the polarization power spectrum. The expected 1 σ error on the measurement of the electron optical depth is around 0.03 with a weak dependence on the value of that optical depth. Such a constraint on the optical depth will allow MAP to achieve a 1 σ error on the amplitude of the primordial power spectrum of 6%. MAP with 2 yr (Planck with 1 yr) of observation can distinguish a model with 50% (6%) partial ionization between redshifts of 6.3 and 20 from a model in which hydrogen was completely neutral at redshifts greater than 6.3. Planck will be able to distinguish between different reionization histories even when they imply the same optical depth to electron scattering for the CMB photons. article_processing_charge: No article_type: original author: - first_name: Manoj full_name: Kaplinghat, Manoj last_name: Kaplinghat - first_name: Mike full_name: Chu, Mike last_name: Chu - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Gilbert P. full_name: Holder, Gilbert P. last_name: Holder - first_name: Lloyd full_name: Knox, Lloyd last_name: Knox - first_name: Constantinos full_name: Skordis, Constantinos last_name: Skordis citation: ama: Kaplinghat M, Chu M, Haiman Z, Holder GP, Knox L, Skordis C. Probing the reionization history of the universe using the cosmic microwave background polarization. The Astrophysical Journal. 2003;583(1):24-32. doi:10.1086/344927 apa: Kaplinghat, M., Chu, M., Haiman, Z., Holder, G. P., Knox, L., & Skordis, C. (2003). Probing the reionization history of the universe using the cosmic microwave background polarization. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/344927 chicago: Kaplinghat, Manoj, Mike Chu, Zoltán Haiman, Gilbert P. Holder, Lloyd Knox, and Constantinos Skordis. “Probing the Reionization History of the Universe Using the Cosmic Microwave Background Polarization.” The Astrophysical Journal. American Astronomical Society, 2003. https://doi.org/10.1086/344927. ieee: M. Kaplinghat, M. Chu, Z. Haiman, G. P. Holder, L. Knox, and C. Skordis, “Probing the reionization history of the universe using the cosmic microwave background polarization,” The Astrophysical Journal, vol. 583, no. 1. American Astronomical Society, pp. 24–32, 2003. ista: Kaplinghat M, Chu M, Haiman Z, Holder GP, Knox L, Skordis C. 2003. Probing the reionization history of the universe using the cosmic microwave background polarization. The Astrophysical Journal. 583(1), 24–32. mla: Kaplinghat, Manoj, et al. “Probing the Reionization History of the Universe Using the Cosmic Microwave Background Polarization.” The Astrophysical Journal, vol. 583, no. 1, American Astronomical Society, 2003, pp. 24–32, doi:10.1086/344927. short: M. Kaplinghat, M. Chu, Z. Haiman, G.P. Holder, L. Knox, C. Skordis, The Astrophysical Journal 583 (2003) 24–32. date_created: 2024-09-06T09:25:08Z date_published: 2003-01-20T00:00:00Z date_updated: 2024-09-26T14:15:21Z day: '20' doi: 10.1086/344927 extern: '1' intvolume: ' 583' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/344927 month: '01' oa: 1 oa_version: Published Version page: 24-32 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Probing the reionization history of the universe using the cosmic microwave background polarization type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 583 year: '2003' ... --- _id: '17754' abstract: - lang: eng text: 'The recent discovery of a high optical depth tau to Thomson scattering from the WMAP data implies that significant reionization took place at redshifts z~15. This discovery has important implications for the sources of reionization, and allows, for the first time, constraints to be placed on physical reionization scenarios out to redshift z~20. Using a new suite of semi-analytic reionization models, we show that the high value of tau requires a surprisingly high efficiency epsilon of the first generation of UV sources for injecting ionizing photons into the intergalactic medium. We find that no simple reionization model can be consistent with the combination of the WMAP result with data from the z<6.5 universe. Satisfying both constraints requires either of the following: (i) H_2 molecules form efficiently at z~20, survive feedback processes, and allow UV sources in halos with virial temperatures below Tvir=10^4 K to contribute substantially to reionization, or (ii) the efficiency epsilon in halos with Tvir>10^4K decreased by a factor of ~ 30 between (z~20) and (z~6). We discuss the relevant physical issues to produce either scenario, and argue that both options are viable, and allowed by current data. In detailed models of the reionization history, we find that the evolution of the ionized fractions in the two scenarios have distinctive features that Planck can distinguish at 3 sigma significance. At the high WMAP value for tau, Planck will also be able to provide tight statistical constraints on reionization model parameters, and elucidate much of the physics at the end of the Dark Ages. The sources responsible for the high optical depth discovered by WMAP should be directly detectable out to z~15 by the James Webb Space Telescope.' article_processing_charge: No article_type: original author: - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Gilbert P. full_name: Holder, Gilbert P. last_name: Holder citation: ama: Haiman Z, Holder GP. The reionization history at high redshifts. I. Physical models and new constraints from cosmic microwave background polarization. The Astrophysical Journal. 2003;595(1):1-12. doi:10.1086/377337 apa: Haiman, Z., & Holder, G. P. (2003). The reionization history at high redshifts. I. Physical models and new constraints from cosmic microwave background polarization. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/377337 chicago: Haiman, Zoltán, and Gilbert P. Holder. “The Reionization History at High Redshifts. I. Physical Models and New Constraints from Cosmic Microwave Background Polarization.” The Astrophysical Journal. American Astronomical Society, 2003. https://doi.org/10.1086/377337. ieee: Z. Haiman and G. P. Holder, “The reionization history at high redshifts. I. Physical models and new constraints from cosmic microwave background polarization,” The Astrophysical Journal, vol. 595, no. 1. American Astronomical Society, pp. 1–12, 2003. ista: Haiman Z, Holder GP. 2003. The reionization history at high redshifts. I. Physical models and new constraints from cosmic microwave background polarization. The Astrophysical Journal. 595(1), 1–12. mla: Haiman, Zoltán, and Gilbert P. Holder. “The Reionization History at High Redshifts. I. Physical Models and New Constraints from Cosmic Microwave Background Polarization.” The Astrophysical Journal, vol. 595, no. 1, American Astronomical Society, 2003, pp. 1–12, doi:10.1086/377337. short: Z. Haiman, G.P. Holder, The Astrophysical Journal 595 (2003) 1–12. date_created: 2024-09-06T09:42:24Z date_published: 2003-09-20T00:00:00Z date_updated: 2024-09-30T08:02:54Z day: '20' doi: 10.1086/377337 extern: '1' intvolume: ' 595' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/377337 month: '09' oa: 1 oa_version: Published Version page: 1-12 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: The reionization history at high redshifts. I. Physical models and new constraints from cosmic microwave background polarization type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 595 year: '2003' ... --- _id: '17760' abstract: - lang: eng text: In light of the recent inference of a high optical depth τ to Thomson scattering from the Wilkinson Microwave Anisotropy Probe (WMAP) data, we investigate the effects of extended periods of partial ionization and ask if the value of τ inferred by assuming a single sharp transition is an unbiased estimate. We construct and consider several representative ionization models and evaluate their signatures in the cosmic microwave background (CMB). If τ is estimated with a single sharp transition, we show that there can be a significant bias in the derived value (and, therefore, a bias in σ8 as well). For WMAP noise levels, the bias in τ is smaller than the statistical uncertainty, but for Planck or a cosmic variance limited experiment the τ bias could be much larger than the statistical uncertainties. This bias can be reduced in the ionization models we consider by fitting a slightly more complicated ionization history, such as a two-step ionization process. Assuming this two-step process, we find that the Planck satellite can simultaneously determine the initial redshift of reionization to ±2 and τ to ±0.01. Uncertainty about the ionization history appears to provide a limit of ~0.005 on how well τ can be estimated from CMB polarization data, much better than expected from WMAP but significantly worse than expected from cosmic variance limits. article_processing_charge: No article_type: original author: - first_name: Gilbert P. full_name: Holder, Gilbert P. last_name: Holder - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Manoj full_name: Kaplinghat, Manoj last_name: Kaplinghat - first_name: Lloyd full_name: Knox, Lloyd last_name: Knox citation: ama: Holder GP, Haiman Z, Kaplinghat M, Knox L. The reionization history at high redshifts. II. Estimating the optical depth to Thomson scattering from cosmic microwave background polarization. The Astrophysical Journal. 2003;595(1):13-18. doi:10.1086/377338 apa: Holder, G. P., Haiman, Z., Kaplinghat, M., & Knox, L. (2003). The reionization history at high redshifts. II. Estimating the optical depth to Thomson scattering from cosmic microwave background polarization. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/377338 chicago: Holder, Gilbert P., Zoltán Haiman, Manoj Kaplinghat, and Lloyd Knox. “The Reionization History at High Redshifts. II. Estimating the Optical Depth to Thomson Scattering from Cosmic Microwave Background Polarization.” The Astrophysical Journal. American Astronomical Society, 2003. https://doi.org/10.1086/377338. ieee: G. P. Holder, Z. Haiman, M. Kaplinghat, and L. Knox, “The reionization history at high redshifts. II. Estimating the optical depth to Thomson scattering from cosmic microwave background polarization,” The Astrophysical Journal, vol. 595, no. 1. American Astronomical Society, pp. 13–18, 2003. ista: Holder GP, Haiman Z, Kaplinghat M, Knox L. 2003. The reionization history at high redshifts. II. Estimating the optical depth to Thomson scattering from cosmic microwave background polarization. The Astrophysical Journal. 595(1), 13–18. mla: Holder, Gilbert P., et al. “The Reionization History at High Redshifts. II. Estimating the Optical Depth to Thomson Scattering from Cosmic Microwave Background Polarization.” The Astrophysical Journal, vol. 595, no. 1, American Astronomical Society, 2003, pp. 13–18, doi:10.1086/377338. short: G.P. Holder, Z. Haiman, M. Kaplinghat, L. Knox, The Astrophysical Journal 595 (2003) 13–18. date_created: 2024-09-06T09:47:55Z date_published: 2003-09-20T00:00:00Z date_updated: 2024-09-30T08:51:32Z day: '20' doi: 10.1086/377338 extern: '1' intvolume: ' 595' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/377338 month: '09' oa: 1 oa_version: Published Version page: 13-18 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: The reionization history at high redshifts. II. Estimating the optical depth to Thomson scattering from cosmic microwave background polarization type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 595 year: '2003' ... --- _id: '17780' abstract: - lang: eng text: We study contributions from inhomogeneous (patchy) reionization to arcminute-scale (1000 < l < 10,000) cosmic microwave background (CMB) anisotropies. We show that inhomogeneities in the ionization fraction, rather than in the mean density, dominate both the temperature and the polarization power spectra. Depending on the ionization history and the clustering bias of the ionizing sources, we find that rms temperature fluctuations range from 2 to 8 μK and the corresponding values for polarization are over 2 orders of magnitude smaller. Reionization can significantly bias cosmological parameter estimates and degrade gravitational lensing potential reconstruction from temperature maps but not from polarization maps. We demonstrate that a simple modeling of the reionization temperature power spectrum may be sufficient to remove the parameter bias. The high-l temperature power spectrum will contain some limited information about the sources of reionization. article_processing_charge: No article_type: original author: - first_name: Mario G. full_name: Santos, Mario G. last_name: Santos - first_name: Asantha full_name: Cooray, Asantha last_name: Cooray - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Lloyd full_name: Knox, Lloyd last_name: Knox - first_name: Chung‐Pei full_name: Ma, Chung‐Pei last_name: Ma citation: ama: Santos MG, Cooray A, Haiman Z, Knox L, Ma C. Small‐scale cosmic microwave background temperature and polarization anisotropies due to patchy reionization. The Astrophysical Journal. 2003;598(2):756-766. doi:10.1086/378772 apa: Santos, M. G., Cooray, A., Haiman, Z., Knox, L., & Ma, C. (2003). Small‐scale cosmic microwave background temperature and polarization anisotropies due to patchy reionization. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/378772 chicago: Santos, Mario G., Asantha Cooray, Zoltán Haiman, Lloyd Knox, and Chung‐Pei Ma. “Small‐scale Cosmic Microwave Background Temperature and Polarization Anisotropies Due to Patchy Reionization.” The Astrophysical Journal. American Astronomical Society, 2003. https://doi.org/10.1086/378772. ieee: M. G. Santos, A. Cooray, Z. Haiman, L. Knox, and C. Ma, “Small‐scale cosmic microwave background temperature and polarization anisotropies due to patchy reionization,” The Astrophysical Journal, vol. 598, no. 2. American Astronomical Society, pp. 756–766, 2003. ista: Santos MG, Cooray A, Haiman Z, Knox L, Ma C. 2003. Small‐scale cosmic microwave background temperature and polarization anisotropies due to patchy reionization. The Astrophysical Journal. 598(2), 756–766. mla: Santos, Mario G., et al. “Small‐scale Cosmic Microwave Background Temperature and Polarization Anisotropies Due to Patchy Reionization.” The Astrophysical Journal, vol. 598, no. 2, American Astronomical Society, 2003, pp. 756–66, doi:10.1086/378772. short: M.G. Santos, A. Cooray, Z. Haiman, L. Knox, C. Ma, The Astrophysical Journal 598 (2003) 756–766. date_created: 2024-09-06T10:15:03Z date_published: 2003-12-01T00:00:00Z date_updated: 2024-09-30T12:07:47Z day: '01' doi: 10.1086/378772 extern: '1' intvolume: ' 598' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/378772 month: '12' oa: 1 oa_version: Published Version page: 756-766 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Small‐scale cosmic microwave background temperature and polarization anisotropies due to patchy reionization type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 598 year: '2003' ... --- _id: '17723' abstract: - lang: eng text: "The recent discovery of bright quasars around redshift z=6 suggests that black holes (BHs) with masses in excess of 10^9 Msun have already assembled at a very early stage in the evolution of the universe. An alternative interpretation is that these quasars are powered by less massive BHs, but their fluxes are strongly magnified through gravitational lensing by intervening galaxies. Here we analyze the flux distribution of the Ly alpha emission of the quasar with the highest known redshift, SDSS 1030+0524, at z=6.28. We show that this object could not have been magnified by lensing by more than a factor of five. The constraint arises from the large observed size, 30 (comoving) Mpc, of the ionized region around this quasar, and relies crucially only on the assumption that the quasar is embedded in a largely neutral IGM. Based on the line/continuum ratio of SDSS 1030+0524, we argue further that this quasar also cannot be beamed by a significant factor. We conclude that the minimum mass for its resident BH is 4 x 10^8 Msun (for magnification by a factor of five); if the mass is this low, then the quasars had to switch on prior to redshift z=9.\r\nFrom the size of the ionized region, we are also able to place an absolute lower bound on the age of this quasar at t > 2 x 10^7 years." article_processing_charge: No article_type: original author: - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: Renyue full_name: Cen, Renyue last_name: Cen citation: ama: Haiman Z, Cen R. A constraint on the gravitational lensing magnification and age of the redshift z = 6.28 Quasar SDSS 1030+0524. The Astrophysical Journal. 2002;578(2):702-707. doi:10.1086/342610 apa: Haiman, Z., & Cen, R. (2002). A constraint on the gravitational lensing magnification and age of the redshift z = 6.28 Quasar SDSS 1030+0524. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/342610 chicago: Haiman, Zoltán, and Renyue Cen. “A Constraint on the Gravitational Lensing Magnification and Age of the Redshift z = 6.28 Quasar SDSS 1030+0524.” The Astrophysical Journal. American Astronomical Society, 2002. https://doi.org/10.1086/342610. ieee: Z. Haiman and R. Cen, “A constraint on the gravitational lensing magnification and age of the redshift z = 6.28 Quasar SDSS 1030+0524,” The Astrophysical Journal, vol. 578, no. 2. American Astronomical Society, pp. 702–707, 2002. ista: Haiman Z, Cen R. 2002. A constraint on the gravitational lensing magnification and age of the redshift z = 6.28 Quasar SDSS 1030+0524. The Astrophysical Journal. 578(2), 702–707. mla: Haiman, Zoltán, and Renyue Cen. “A Constraint on the Gravitational Lensing Magnification and Age of the Redshift z = 6.28 Quasar SDSS 1030+0524.” The Astrophysical Journal, vol. 578, no. 2, American Astronomical Society, 2002, pp. 702–07, doi:10.1086/342610. short: Z. Haiman, R. Cen, The Astrophysical Journal 578 (2002) 702–707. date_created: 2024-09-06T09:11:03Z date_published: 2002-10-20T00:00:00Z date_updated: 2024-09-25T14:06:28Z day: '20' doi: 10.1086/342610 extern: '1' intvolume: ' 578' issue: '2' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/342610 month: '10' oa: 1 oa_version: Published Version page: 702-707 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: A constraint on the gravitational lensing magnification and age of the redshift z = 6.28 Quasar SDSS 1030+0524 type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 578 year: '2002' ... --- _id: '17739' abstract: - lang: eng text: An extensive sample of galaxy clusters will be available in the coming years, detected through their Sunyaev-Zeldovich effect (SZE). We use a semianalytic model to study the scientific yield of combining SZE data with X-ray and optical follow-up observations. If clusters at a given redshift z0 can be identified with virialized, spherical halos, they populate a well-defined "fundamental plane" (FP) in the parameter space of the three observables virial temperature (T), total Sunyaev-Zeldovich flux decrement (ΔSν), and angular size (θ). The location and orientation of the FP, as well as its redshift evolution, are sensitive to both the internal evolution of clusters and to the underlying cosmological parameters. We show that if clusters are not standard candles (e.g., because of feedback or energy injection), then this can be inferred from the FP. Likewise, we study the dependence of the FP on the cosmological parameters h, σ8, and Ω0, and quantify future constraints on these parameters. We also show that in the absence of any nongravitational effects, the scatter in the (ΔSν,T)-plane is significantly smaller than in either the (θ,T) or the (θ,ΔSν) planes. As a result, the ΔSν-T relation can be an exceptionally sensitive probe of both cluster physics and cosmological parameters. A comparison of the amount of scatter in these three scaling relations will test the origin (cosmological vs. stochastic) of the scatter. article_processing_charge: No article_type: original author: - first_name: Licia full_name: Verde, Licia last_name: Verde - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman - first_name: David N. full_name: Spergel, David N. last_name: Spergel citation: ama: Verde L, Haiman Z, Spergel DN. Are clusters standard candles? Galaxy cluster scaling relations with the Sunyaev‐Zeldovich effect. The Astrophysical Journal. 2002;581(1):5-19. doi:10.1086/344134 apa: Verde, L., Haiman, Z., & Spergel, D. N. (2002). Are clusters standard candles? Galaxy cluster scaling relations with the Sunyaev‐Zeldovich effect. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/344134 chicago: Verde, Licia, Zoltán Haiman, and David N. Spergel. “Are Clusters Standard Candles? Galaxy Cluster Scaling Relations with the Sunyaev‐Zeldovich Effect.” The Astrophysical Journal. American Astronomical Society, 2002. https://doi.org/10.1086/344134. ieee: L. Verde, Z. Haiman, and D. N. Spergel, “Are clusters standard candles? Galaxy cluster scaling relations with the Sunyaev‐Zeldovich effect,” The Astrophysical Journal, vol. 581, no. 1. American Astronomical Society, pp. 5–19, 2002. ista: Verde L, Haiman Z, Spergel DN. 2002. Are clusters standard candles? Galaxy cluster scaling relations with the Sunyaev‐Zeldovich effect. The Astrophysical Journal. 581(1), 5–19. mla: Verde, Licia, et al. “Are Clusters Standard Candles? Galaxy Cluster Scaling Relations with the Sunyaev‐Zeldovich Effect.” The Astrophysical Journal, vol. 581, no. 1, American Astronomical Society, 2002, pp. 5–19, doi:10.1086/344134. short: L. Verde, Z. Haiman, D.N. Spergel, The Astrophysical Journal 581 (2002) 5–19. date_created: 2024-09-06T09:22:05Z date_published: 2002-12-10T00:00:00Z date_updated: 2024-09-26T14:09:02Z day: '10' doi: 10.1086/344134 extern: '1' intvolume: ' 581' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/344134 month: '12' oa: 1 oa_version: Published Version page: 5-19 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: Are clusters standard candles? Galaxy cluster scaling relations with the Sunyaev‐Zeldovich effect type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 581 year: '2002' ... --- _id: '17746' abstract: - lang: eng text: For a source of Lyα radiation embedded in a neutral intergalactic medium (IGM) prior to the reionization epoch, the Lyα emission line is strongly suppressed by the intervening IGM. The damping wing of the so-called Gunn-Peterson trough can extend to the red side of the emission line and erase a significant fraction of the total line flux. However, the transmitted fraction increases with the size of the local cosmological H II region surrounding the source, and therefore with the ionizing luminosity and age of the source. Motivated by the recent discovery of a Lyα-emitting galaxy at a redshift z = 6.56 (Hu et al.), possibly prior to the reionization of the IGM, we revisit the effects of a neutral IGM on the Lyα emission line. We show that for faint sources with little or even no ionizing continuum, a sufficiently broad (Δv ≳ 300 km s^-1) emission line can still remain observable. In particular, the line detected by Hu et al. is consistent with a source embedded in a neutral IGM. We provide characterizations of the asymmetry and total transmitted flux of the Lyα line as functions of the ionizing emissivity of its source. We argue that a statistical sample of Lyα emitters extending beyond the reionization redshift can be a useful probe of reionization. article_processing_charge: No article_type: original author: - first_name: Zoltán full_name: Haiman, Zoltán id: 7c006e8c-cc0d-11ee-8322-cb904ef76f36 last_name: Haiman citation: ama: Haiman Z. The detectability of high-redshift Lyα emission lines prior to the reionization of the universe. The Astrophysical Journal. 2002;576(1):L1-L4. doi:10.1086/343101 apa: Haiman, Z. (2002). The detectability of high-redshift Lyα emission lines prior to the reionization of the universe. The Astrophysical Journal. American Astronomical Society. https://doi.org/10.1086/343101 chicago: Haiman, Zoltán. “The Detectability of High-Redshift Lyα Emission Lines Prior to the Reionization of the Universe.” The Astrophysical Journal. American Astronomical Society, 2002. https://doi.org/10.1086/343101. ieee: Z. Haiman, “The detectability of high-redshift Lyα emission lines prior to the reionization of the universe,” The Astrophysical Journal, vol. 576, no. 1. American Astronomical Society, pp. L1–L4, 2002. ista: Haiman Z. 2002. The detectability of high-redshift Lyα emission lines prior to the reionization of the universe. The Astrophysical Journal. 576(1), L1–L4. mla: Haiman, Zoltán. “The Detectability of High-Redshift Lyα Emission Lines Prior to the Reionization of the Universe.” The Astrophysical Journal, vol. 576, no. 1, American Astronomical Society, 2002, pp. L1–4, doi:10.1086/343101. short: Z. Haiman, The Astrophysical Journal 576 (2002) L1–L4. date_created: 2024-09-06T09:34:46Z date_published: 2002-07-31T00:00:00Z date_updated: 2024-09-26T14:51:17Z day: '31' doi: 10.1086/343101 extern: '1' intvolume: ' 576' issue: '1' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.1086/343101 month: '07' oa: 1 oa_version: Published Version page: L1-L4 publication: The Astrophysical Journal publication_identifier: issn: - 0004-637X - 1538-4357 publication_status: published publisher: American Astronomical Society quality_controlled: '1' scopus_import: '1' status: public title: The detectability of high-redshift Lyα emission lines prior to the reionization of the universe type: journal_article user_id: 317138e5-6ab7-11ef-aa6d-ffef3953e345 volume: 576 year: '2002' ...