[ { "id": "authors:q0jbp-fhd85", "collection": "authors", "collection_id": "q0jbp-fhd85", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091102-131150092", "type": "article", "title": "The 6dF Galaxy Survey: final redshift release (DR3) and southern large-scale structures", "author": [ { "family_name": "Jones", "given_name": "D. Heath", "clpid": "Jones-D-H" }, { "family_name": "Read", "given_name": "Mike A.", "clpid": "Read-M-A" }, { "family_name": "Saunders", "given_name": "Will", "clpid": "Saunders-W" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Jarrett", "given_name": "Tom", "clpid": "Jarrett-T" }, { "family_name": "Parker", "given_name": "Quentin A.", "clpid": "Parker-Q-A" }, { "family_name": "Fairall", "given_name": "Anthony P.", "clpid": "Fairall-A-P" }, { "family_name": "Mauch", "given_name": "Thomas", "clpid": "Mauch-T" }, { "family_name": "Sadler", "given_name": "Elaine M.", "clpid": "Sadler-E-M" }, { "family_name": "Watson", "given_name": "Fred G.", "clpid": "Watson-F-G" }, { "family_name": "Burton", "given_name": "Donna", "clpid": "Burton-D" }, { "family_name": "Campbell", "given_name": "Lachlan A.", "clpid": "Campbell-L-A" }, { "family_name": "Cass", "given_name": "Paul", "clpid": "Cass-P" }, { "family_name": "Croom", "given_name": "Scott M.", "orcid": "0000-0003-2880-9197", "clpid": "Croom-S-M" }, { "family_name": "Dawe", "given_name": "John", "clpid": "Dawe-J" }, { "family_name": "Fiegert", "given_name": "Kristin", "clpid": "Fiegert-K" }, { "family_name": "Frankcombe", "given_name": "Leela", "clpid": "Frankcombe-L" }, { "family_name": "Hartley", "given_name": "Malcolm", "clpid": "Hartley-Malcolm" }, { "family_name": "Huchra", "given_name": "John", "clpid": "Huchra-J-P" }, { "family_name": "James", "given_name": "Dionne", "clpid": "James-D" }, { "family_name": "Kirby", "given_name": "Emma", "clpid": "Kirby-Emma" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lucey", "given_name": "John", "clpid": "Lucey-J" }, { "family_name": "Mamon", "given_name": "Gary A.", "clpid": "Mamon-G-A" }, { "family_name": "Moore", "given_name": "Lesa", "clpid": "Moore-L" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Prior", "given_name": "Sayuri", "clpid": "Prior-S" }, { "family_name": "Proust", "given_name": "Dominique", "clpid": "Proust-D" }, { "family_name": "Russell", "given_name": "Ken", "clpid": "Russell-K" }, { "family_name": "Safouris", "given_name": "Vicky", "clpid": "Safouris-V" }, { "family_name": "Wakamatsu", "given_name": "Ken-ichi", "clpid": "Wakamatsu-K" }, { "family_name": "Westra", "given_name": "Eduard", "clpid": "Westra-E" }, { "family_name": "Williams", "given_name": "Mary", "clpid": "Williams-M" } ], "abstract": "We report the final redshift release of the 6dF Galaxy Survey (6dFGS), a combined redshift and peculiar velocity survey over the southern sky (|b| > 10\u00b0). Its 136 304 spectra have yielded 110 256 new extragalactic redshifts and a new catalogue of 125 071 galaxies making near-complete samples with (K, H, J, r_F, b_J) \u2264 (12.65, 12.95, 13.75, 15.60, 16.75). The median redshift of the survey is 0.053. Survey data, including images, spectra, photometry and redshifts, are available through an online data base. We describe changes to the information in the data base since earlier interim data releases. Future releases will include velocity dispersions, distances and peculiar velocities for the brightest early-type galaxies, comprising about 10 per cent of the sample. Here we provide redshift maps of the southern local Universe with z \u2264 0.1, showing nearby large-scale structures in hitherto unseen detail. A number of regions known previously to have a paucity of galaxies are confirmed as significantly underdense regions. The URL of the 6dFGS data base is http://www-wfau.roe.ac.uk/6dFGS.", "doi": "10.1111/j.1365-2966.2009.15338.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2009-10-21", "series_number": "2", "volume": "399", "issue": "2", "pages": "683-698" }, { "id": "authors:7edch-wh733", "collection": "authors", "collection_id": "7edch-wh733", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20090618-204832185", "type": "article", "title": "A comprehensive study of GRB 070125, a most energetic gamma-ray burst", "author": [ { "family_name": "Chandra", "given_name": "Poonam", "clpid": "Chandra-P" }, { "family_name": "Cenko", "given_name": "S. Bradley", "orcid": "0000-0003-1673-970X", "clpid": "Cenko-S-B" }, { "family_name": "Frail", "given_name": "Dale A.", "clpid": "Frail-D-A" }, { "family_name": "Chevalier", "given_name": "Roger A.", "clpid": "Chevalier-R-A" }, { "family_name": "Macquart", "given_name": "Jean-Pierre R.", "orcid": "0000-0001-6763-8234", "clpid": "Macquart-J-P" }, { "family_name": "Kulkarni", "given_name": "Shri R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Bock", "given_name": "Douglas C.-J.", "clpid": "Bock-D-C-J" }, { "family_name": "Bertoldi", "given_name": "Frank", "orcid": "0000-0002-1707-1775", "clpid": "Bertoldi-F" }, { "family_name": "Kasliwal", "given_name": "Mansi", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Fox", "given_name": "Derek B.", "orcid": "0000-0002-3714-672X", "clpid": "Fox-D-B" }, { "family_name": "Price", "given_name": "Paul A.", "clpid": "Price-P-A" }, { "family_name": "Berger", "given_name": "Edo", "orcid": "0000-0002-9392-9681", "clpid": "Berger-Edo" }, { "family_name": "Soderberg", "given_name": "Alicia M.", "clpid": "Soderberg-A-M" }, { "family_name": "Harrison", "given_name": "Fiona A.", "orcid": "0000-0002-4226-8959", "clpid": "Harrison-F-A" }, { "family_name": "Gal-Yam", "given_name": "Avishay", "orcid": "0000-0002-3653-5598", "clpid": "Gal-Yam-A" }, { "family_name": "Ofek", "given_name": "Eran O.", "orcid": "0000-0002-6786-8774", "clpid": "Ofek-E-O" }, { "family_name": "Rau", "given_name": "Arne", "orcid": "0000-0001-5990-6243", "clpid": "Rau-A" }, { "family_name": "Schmidt", "given_name": "Brian P.", "orcid": "0000-0001-6589-1287", "clpid": "Schmidt-B-P" }, { "family_name": "Cameron", "given_name": "P. Brian", "clpid": "Cameron-P-B" }, { "family_name": "Cowie", "given_name": "Lennox L.", "orcid": "0000-0002-6319-1575", "clpid": "Cowie-L-L" }, { "family_name": "Cowie", "given_name": "Antionette", "clpid": "Cowie-A" }, { "family_name": "Roth", "given_name": "Katherine C.", "clpid": "Roth-K-C" }, { "family_name": "Dopita", "given_name": "Michael", "clpid": "Dopita-M-A" }, { "family_name": "Peterson", "given_name": "Bruce", "clpid": "Peterson-B-A" }, { "family_name": "Penprase", "given_name": "Bryan E.", "clpid": "Penprase-B-E" } ], "abstract": "We present a comprehensive multiwavelength analysis of the bright, long-duration gamma-ray burst GRB 070125, comprised of observations in gamma-ray, X-ray, optical, millimeter, and centimeter wave bands. Simultaneous fits to the optical and X-ray light curves favor a break on day 3.78, which we interpret as the jet break from a collimated outflow. Independent fits to optical and X-ray bands give similar results in the optical bands but shift the jet break to around day 10 in the X-ray light curve. We show that for the physical parameters derived for GRB 070125, inverse Compton scattering effects are important throughout the afterglow evolution. While inverse Compton scattering does not affect radio and optical bands, it may be a promising candidate to delay the jet break in the X-ray band. Radio light curves show rapid flux variations, which are interpreted as due to interstellar scintillation and used to derive an upper limit of 2.4 \u00d7 10^(17) cm on the radius of the fireball in the lateral expansion phase of the jet. Radio light curves and spectra suggest a high synchrotron self-absorption frequency indicative of the afterglow shock wave moving in a dense medium. Our broadband modeling favors a constant density profile for the circumburst medium over a windlike profile (R^(\u22122)). However, keeping in mind the uncertainty of the parameters, it is difficult to unambiguously distinguish between the two density profiles. Our broadband fits suggest that GRB 070125 is a burst with high radiative efficiency (>60%).", "doi": "10.1086/589807", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2008-08-20", "series_number": "2", "volume": "689", "issue": "2", "pages": "924-942" }, { "id": "authors:wz2bk-6a741", "collection": "authors", "collection_id": "wz2bk-6a741", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091016-151324786", "type": "article", "title": "Hubble Space Telescope and Spitzer Observations of the Afterglow and Host Galaxy of GRB 050904 at z = 6.295", "author": [ { "family_name": "Berger", "given_name": "E.", "orcid": "0000-0002-9392-9681", "clpid": "Berger-Edo" }, { "family_name": "Chary", "given_name": "R.", "orcid": "0000-0001-7583-0621", "clpid": "Chary-R-R" }, { "family_name": "Cowie", "given_name": "L. L.", "orcid": "0000-0002-6319-1575", "clpid": "Cowie-L-L" }, { "family_name": "Price", "given_name": "P. A.", "clpid": "Price-P-A" }, { "family_name": "Schmidt", "given_name": "B. P.", "orcid": "0000-0001-6589-1287", "clpid": "Schmidt-B-P" }, { "family_name": "Fox", "given_name": "D. B.", "orcid": "0000-0002-3714-672X", "clpid": "Fox-D-B" }, { "family_name": "Cenko", "given_name": "S. B.", "orcid": "0000-0003-1673-970X", "clpid": "Cenko-S-B" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Soderberg", "given_name": "A. M.", "clpid": "Soderberg-A-M" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "McCarthy", "given_name": "P. J.", "clpid": "McCarthy-P-J" }, { "family_name": "Gladders", "given_name": "M. D.", "clpid": "Gladders-M-D" }, { "family_name": "Peterson", "given_name": "B. A.", "clpid": "Peterson-B-A" }, { "family_name": "Barger", "given_name": "A. J.", "orcid": "0000-0002-3306-1606", "clpid": "Barger-A-J" } ], "abstract": "We present deep Hubble Space Telescope (HST ) and Spitzer Space Telescope observations of GRB 050904 at z = 6:295. We detect the afterglow in the H band more than 3 weeks after the burst and confirm the presence of a jet break at t \u2248 2:1 days. This leads to an estimated opening angle of about 4\u00b0 and a beaming-corrected energy of about 10^(51) ergs, similar to those of lower redshift gamma-ray bursts (GRBs). We do not detect an underlying host galaxy with either HST or Spitzer. From the upper limits we infer an extinction-corrected absolute magnitude M_(UV) \u2273 -20:3 mag, or L \u227e L^*, a star formation rate of \u227e 5.7M_\u2299 yr^(-1), and a stellar mass of \u227e few x 10^9 M_\u2299. A comparison to spectroscopically confirmed galaxies at z > 5:5 reveals that the host of GRB 050904 is fainter and has a lower star formation rate than at least 80% of these objects. Finally, using our luminosity limits, and the metallicity of about 0.05 Z_\u2299 inferred from the afterglow absorption spectrum, we place the first limit on the luminosity-metallicity relation at z > 6. Future afterglow and host galaxy observations of z \u2273 4 GRBs should elucidate whether the mass- and luminosity-metallicity relations continue to evolve beyond the present limits of z \u227e 2.", "doi": "10.1086/519511", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2007-08-10", "series_number": "1", "volume": "665", "issue": "1", "pages": "102-106" }, { "id": "authors:5y6ek-zj956", "collection": "authors", "collection_id": "5y6ek-zj956", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20091026-162635451", "type": "article", "title": "A New Population of High-Redshift Short-Duration Gamma-Ray Bursts", "author": [ { "family_name": "Berger", "given_name": "E.", "orcid": "0000-0002-9392-9681", "clpid": "Berger-Edo" }, { "family_name": "Fox", "given_name": "D. B.", "orcid": "0000-0002-3714-672X", "clpid": "Fox-D-B" }, { "family_name": "Price", "given_name": "P. A.", "clpid": "Price-P-A" }, { "family_name": "Nakar", "given_name": "E.", "orcid": "0000-0002-4534-7089", "clpid": "Nakar-E" }, { "family_name": "Gal-Yam", "given_name": "A.", "orcid": "0000-0002-3653-5598", "clpid": "Gal-Yam-A" }, { "family_name": "Holz", "given_name": "D. E.", "clpid": "Holz-D-E" }, { "family_name": "Schmidt", "given_name": "B. P.", "orcid": "0000-0001-6589-1287", "clpid": "Schmidt-B-P" }, { "family_name": "Cucchiara", "given_name": "A.", "clpid": "Cucchiara-A" }, { "family_name": "Cenko", "given_name": "S. B.", "orcid": "0000-0003-1673-970X", "clpid": "Cenko-S-B" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Soderberg", "given_name": "A. M.", "clpid": "Soderberg-A-M" }, { "family_name": "Frail", "given_name": "D. A.", "clpid": "Frail-D-A" }, { "family_name": "Penprase", "given_name": "B. E.", "clpid": "Penprase-B-E" }, { "family_name": "Rau", "given_name": "A.", "orcid": "0000-0001-5990-6243", "clpid": "Rau-A" }, { "family_name": "Ofek", "given_name": "E.", "orcid": "0000-0002-6786-8774", "clpid": "Ofek-E-O" }, { "family_name": "Bell-Burnell", "given_name": "S. J.", "clpid": "Bell-Burnell-S-J" }, { "family_name": "Cameron", "given_name": "P. B.", "clpid": "Cameron-P-B" }, { "family_name": "Cowie", "given_name": "L. L.", "orcid": "0000-0002-6319-1575", "clpid": "Cowie-L-L" }, { "family_name": "Dopita", "given_name": "M. A.", "clpid": "Dopita-M-A" }, { "family_name": "Hook", "given_name": "I.", "orcid": "0000-0002-2960-978X", "clpid": "Hook-I-M" }, { "family_name": "Peterson", "given_name": "B. A.", "clpid": "Peterson-B-A" }, { "family_name": "Podsiadlowski", "given_name": "P.", "clpid": "Podsiadlowski-P" }, { "family_name": "Roth", "given_name": "K. C.", "clpid": "Roth-K-C" }, { "family_name": "Rutledge", "given_name": "R. E.", "clpid": "Rutledge-R-E" }, { "family_name": "Sheppard", "given_name": "S. S.", "orcid": "0000-0003-3145-8682", "clpid": "Sheppard-S-S" }, { "family_name": "Songaila", "given_name": "A.", "clpid": "Songaila-A" } ], "abstract": "The redshift distribution of the short-duration gamma-ray bursts (GRBs) is a crucial, but currently fragmentary, clue to the nature of their progenitors. Here we present optical observations of nine short GRBs obtained with Gemini, Magellan, and the Hubble Space Telescope. We detect the afterglows and host galaxies of two short bursts, and host galaxies for two additional bursts with known optical afterglow positions, and five with X-ray positions (\u22726\" radius). In eight of the nine cases we find that the most probable host galaxies are faint, R \u2248 23-26.5 mag, and are therefore starkly different from the first few short GRB hosts with R \u2248 17-22 mag and z \u2272 0.5. Indeed, we measure spectroscopic redshifts of z \u2248 0.4-1.1 for the four brightest hosts. A comparison to large field galaxy samples, as well as the hosts of long GRBs and previous short GRBs, indicates that the fainter hosts likely reside at z \u2273 1. Our most conservative limit is that at least half of the five hosts without a known redshift reside at z > 0.7 (97% confidence level), suggesting that about 1/3 to 2/3 of all short GRBs originate at higher redshifts than previously determined. This has two important implications: (1) we constrain the acceptable age distributions to a wide lognormal (\u03c3 \u2273 1) with \u03c4* ~ 4-8 Gyr, or to a power law, P(\u03c4)\u03b1 \u03c4^n, with -1 \u2272 n \u2272 0; and (2) the inferred isotropic energies, E_\u03b3,iso ~ 10^50-10^52 ergs, are significantly larger than ~10^48-10^49 ergs for the low-redshift, short GRBs, indicating a large spread in energy release or jet opening angles. Finally, we reiterate the importance of short GRBs as potential gravitational-wave sources and find a conservative detection rate with the advanced Laser Interferometer Gravitational-Wave Observatory (LIGO) of ~2-6 yr^-1.", "doi": "10.1086/518762", "issn": "0004-637X", "publisher": "American Astronomical Society", "publication": "Astrophysical Journal", "publication_date": "2007-08-01", "series_number": "2", "volume": "664", "issue": "2", "pages": "1000-1010" }, { "id": "authors:y1qnw-y4w37", "collection": "authors", "collection_id": "y1qnw-y4w37", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150331-092218774", "type": "article", "title": "The afterglow and elliptical host galaxy of the short big \u03b3-ray burst GRB 050724", "author": [ { "family_name": "Berger", "given_name": "E.", "orcid": "0000-0002-9392-9681", "clpid": "Berger-Edo" }, { "family_name": "Price", "given_name": "P. A.", "clpid": "Price-P-A" }, { "family_name": "Cenko", "given_name": "S. B.", "orcid": "0000-0003-1673-970X", "clpid": "Cenko-S-B" }, { "family_name": "Gal-Yam", "given_name": "A.", "orcid": "0000-0002-3653-5598", "clpid": "Gal-Yam-A" }, { "family_name": "Soderberg", "given_name": "A. M.", "clpid": "Soderberg-A-M" }, { "family_name": "Kasliwal", "given_name": "M. M.", "orcid": "0000-0002-5619-4938", "clpid": "Kasliwal-M-M" }, { "family_name": "Leonard", "given_name": "D. C.", "clpid": "Leonard-D-C" }, { "family_name": "Cameron", "given_name": "P. B.", "clpid": "Cameron-P-B" }, { "family_name": "Frail", "given_name": "D. A.", "clpid": "Frail-D-A" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Murphy", "given_name": "D. C.", "clpid": "Murphy-D-C" }, { "family_name": "Krzeminski", "given_name": "W.", "clpid": "Krzeminski-W" }, { "family_name": "Piran", "given_name": "T.", "orcid": "0000-0002-7964-5420", "clpid": "Piran-T" }, { "family_name": "Lee", "given_name": "B. L.", "clpid": "Lee-B-L" }, { "family_name": "Roth", "given_name": "K. C.", "clpid": "Roth-K-C" }, { "family_name": "Moon", "given_name": "D. S.", "orcid": "0000-0003-4200-5064", "clpid": "Moon-Dae-Sik" }, { "family_name": "Fox", "given_name": "D. B.", "orcid": "0000-0002-3714-672X", "clpid": "Fox-D-B" }, { "family_name": "Harrison", "given_name": "F. A.", "orcid": "0000-0002-4226-8959", "clpid": "Harrison-F-A" }, { "family_name": "Persson", "given_name": "S. E. E.", "clpid": "Persson-S-E" }, { "family_name": "Schmidt", "given_name": "B. P.", "orcid": "0000-0001-6589-1287", "clpid": "Schmidt-B-P" }, { "family_name": "Penprase", "given_name": "B. E.", "clpid": "Penprase-B-E" }, { "family_name": "Rich", "given_name": "J.", "orcid": "0000-0002-5807-5078", "clpid": "Rich-J-A" }, { "family_name": "Peterson", "given_name": "B. A.", "clpid": "Peterson-B-A" }, { "family_name": "Cowie", "given_name": "L. L.", "orcid": "0000-0002-6319-1575", "clpid": "Cowie-L-L" } ], "abstract": "Despite a rich phenomenology, \u03b3-ray bursts (GRBs) are divided1 into two classes based on their duration and spectral hardness\u2014the long-soft and the short-hard bursts. The discovery of afterglow emission from long GRBs was a watershed event, pinpointing their origin to star-forming galaxies, and hence the death of massive stars, and indicating an energy release of about 10^(51) erg. While theoretical arguments suggest that short GRBs are produced in the coalescence of binary compact objects (neutron stars or black holes), the progenitors, energetics and environments of these events remain elusive despite recent localizations. Here we report the discovery of the first radio afterglow from the short burst GRB 050724, which unambiguously associates it with an elliptical galaxy at a redshift z = 0.257. We show that the burst is powered by the same relativistic fireball mechanism as long GRBs, with the ejecta possibly collimated in jets, but that the total energy release is 10\u20131,000 times smaller. More importantly, the nature of the host galaxy demonstrates that short GRBs arise from an old (> 1 Gyr) stellar population, strengthening earlier suggestions and providing support for coalescing compact object binaries as the progenitors.", "doi": "10.1038/nature04238", "issn": "0028-0836", "publisher": "Nature Publishing Group", "publication": "Nature", "publication_date": "2005-12-15", "series_number": "7070", "volume": "438", "issue": "7070", "pages": "988-990" }, { "id": "authors:40e65-phy40", "collection": "authors", "collection_id": "40e65-phy40", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200708-151733389", "type": "article", "title": "Galaxy ecology: groups and low-density environments in the SDSS and 2dFGRS", "author": [ { "family_name": "Balogh", "given_name": "Michael", "clpid": "Balogh-M-L" }, { "family_name": "Eke", "given_name": "Vince", "clpid": "Eke-V-R" }, { "family_name": "Miller", "given_name": "Chris", "clpid": "Miller-Christopher" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Bower", "given_name": "Richard", "clpid": "Bower-R-G" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Nichol", "given_name": "Robert", "clpid": "Nichol-R-C" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Baldry", "given_name": "Ivan K.", "clpid": "Baldry-I-K" }, { "family_name": "Baugh", "given_name": "Carlton", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Cross", "given_name": "Nicholas", "clpid": "Cross-N-J-G" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G-B" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Gomez", "given_name": "Percy", "clpid": "Gomez-Percy" }, { "family_name": "Gray", "given_name": "Alex", "clpid": "Gray-A-G" }, { "family_name": "Hawkins", "given_name": "Edward", "clpid": "Hawkins-E" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Madgwick", "given_name": "Darren", "clpid": "Madgwick-D-S" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Percival", "given_name": "Will", "clpid": "Percival-W-J" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" } ], "abstract": "We analyse the observed correlation between galaxy environment and H\u03b1 emission-line strength, using volume-limited samples and group catalogues of 24 968 galaxies at 0.05 < z < 0.095, drawn from the 2dF Galaxy Redshift Survey (M_(bJ) < \u221219.5) and the Sloan Digital Sky Survey (M\u1d63 < \u221220.6). We characterize the environment by: (1) \u03a3\u2085, the surface number density of galaxies determined by the projected distance to the fifth nearest neighbour; and (2) \u03c11.1 and \u03c15.5, three-dimensional density estimates obtained by convolving the galaxy distribution with Gaussian kernels of dispersion 1.1 and 5.5 Mpc, respectively. We find that star-forming and quiescent galaxies form two distinct populations, as characterized by their H\u03b1 equivalent width, W\u2080(H\u03b1). The relative numbers of star-forming and quiescent galaxies vary strongly and continuously with local density. However, the distribution of W\u2080(H\u03b1) amongst the star-forming population is independent of environment. The fraction of star-forming galaxies shows strong sensitivity to the density on large scales, \u03c15.5, which is likely independent of the trend with local density, \u03c11.1.We use two differently selected group catalogues to demonstrate that the correlation with galaxy density is approximately independent of group velocity dispersion, for \u03c3 = 200\u20131000 km s\u207b\u00b9. Even in the lowest-density environments, no more than \u223c70 per cent of galaxies show significant H\u03b1 emission. Based on these results, we conclude that the present-day correlation between star formation rate and environment is a result of short-time-scale mechanisms that take place preferentially at high redshift, such as starbursts induced by galaxy\u2013galaxy interactions.", "doi": "10.1111/j.1365-2966.2004.07453.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2004-03-11", "series_number": "4", "volume": "348", "issue": "4", "pages": "1355-1372" }, { "id": "authors:s0h1t-yvm40", "collection": "authors", "collection_id": "s0h1t-yvm40", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200708-151733246", "type": "article", "title": "Galaxy groups in the 2dFGRS: the group-finding algorithm and the 2PIGG catalogue", "author": [ { "family_name": "Eke", "given_name": "V. R.", "clpid": "Eke-V-R" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Baldry", "given_name": "Ivan K.", "clpid": "Baldry-I-K" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G-B" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Madgwick", "given_name": "Darren", "clpid": "Madgwick-D-S" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" }, { "literal": "2dFGRS Team" } ], "abstract": "The construction of a catalogue of galaxy groups from the Two-degree Field Galaxy Redshift Survey (2dFGRS) is described. Groups are identified by means of a friends-of-friends percolation algorithm which has been thoroughly tested on mock versions of the 2dFGRS generated from cosmological N-body simulations. The tests suggest that the algorithm groups all galaxies that it should be grouping, with an additional 40 per cent of interlopers. About 55 per cent of the \u223c190 000 galaxies considered are placed into groups containing at least two members of which \u223c29 000 are found. Of these, \u223c7000 contain at least four galaxies, and these groups have a median redshift of 0.11 and a median velocity dispersion of 260 km s\u207b\u00b9. This 2dFGRS Percolation-Inferred Galaxy Group (2PIGG) catalogue represents the largest available homogeneous sample of galaxy groups. It is publicly available on the World Wide Web.", "doi": "10.1111/j.1365-2966.2004.07408.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2004-03-01", "series_number": "3", "volume": "348", "issue": "3", "pages": "866-878" }, { "id": "authors:1n4mz-3kk30", "collection": "authors", "collection_id": "1n4mz-3kk30", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200708-151733120", "type": "article", "title": "The 2dF Galaxy Redshift Survey: correlation functions, peculiar velocities and the matter density of the Universe", "author": [ { "family_name": "Hawkins", "given_name": "Ed", "clpid": "Hawkins-E" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Madgwick", "given_name": "Darren S.", "clpid": "Madgwick-D-S" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Baldry", "given_name": "Ivan K.", "clpid": "Baldry-I-K" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Jones", "given_name": "Bryn", "clpid": "Jones-Bryn" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Percival", "given_name": "Will", "clpid": "Percival-W" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" }, { "literal": "2dFGRS Team" } ], "abstract": "We present a detailed analysis of the two-point correlation function, \u03be (\u03c3, \u03c0), from the 2dFGalaxy Redshift Survey (2dFGRS). The large size of the catalogue, which contains \u223c220 000 redshifts, allows us to make high-precision measurements of various properties of the galaxy clustering pattern. The effective redshift at which our estimates are made is z\u209b \u2248 0.15, and similarly the effective luminosity, L\u209b \u2248 1.4L\u2217. We estimate the redshift-space correlation function, \u03be (s), from which we measure the redshift-space clustering length, s\u2080 = 6.82 \u00b1 0.28 h\u207b\u00b9 Mpc. We also estimate the projected correlation function, \u039e(\u03c3), and the real-space correlation function, \u03be (r ), which can be fit by a power law (r/r\u2080)\u2212\u03b3 r\u2080 , with r\u2080 = 5.05 \u00b1 0.26 h\u207b\u00b9 Mpc, \u03b3 r = 1.67 \u00b1 0.03. For r \u2273 20 h\u207b\u00b9 Mpc, \u03be drops below a power law as, for instance, is expected in the popular \u039b cold dark matter model. The ratio of amplitudes of the real- and redshift-space correlation functions on scales of 8\u201330 h\u207b\u00b9 Mpc gives an estimate of the redshift-space distortion parameter \u03b2. The quadrupole moment of \u03be (\u03c3, \u03c0) on scales 30\u201340 h\u207b\u00b9 Mpc provides another estimate of \u03b2. We also estimate the distribution function of pairwise peculiar velocities, f (v), including rigorously the significant effect due to the infall velocities, and we find that the distribution is well fit by an exponential form. The accuracy of our \u03be (\u03c3, \u03c0) measurement is sufficient to constrain a model, which simultaneously fits the shape and amplitude of \u03be (r) and the two redshift-space distortion effects parametrized by \u03b2 and velocity dispersion, a. We find \u03b2 = 0.49 \u00b1 0.09 and a= 506 \u00b1 52 km s\u207b\u00b9, although the best-fitting values are strongly correlated. We measure the variation of the peculiar velocity dispersion with projected separation, a(\u03c3), and find that the shape is consistent with models and simulations. This is the first time that \u03b2 and \u0192(v) have been estimated from a self-consistent model of galaxy velocities. Using the constraints on bias from recent estimates, and taking account of redshift evolution, we conclude that \u03b2 (L=L*, z= 0) = 0.47 \u00b1 0.08, and that the present-day matter density of the Universe, \u03a9_m\u2248 0.3, consistent with other 2dFGRS estimates and independent analyses.", "doi": "10.1046/j.1365-2966.2003.07063.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2003-11-21", "series_number": "1", "volume": "346", "issue": "1", "pages": "78-96" }, { "id": "authors:n70zy-vhb68", "collection": "authors", "collection_id": "n70zy-vhb68", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200629-094519564", "type": "article", "title": "The 2dF Galaxy Redshift Survey: galaxy clustering per spectral type", "author": [ { "family_name": "Madgwick", "given_name": "Darren S.", "clpid": "Madgwick-D-S" }, { "family_name": "Hawkins", "given_name": "Ed", "clpid": "Hawkins-E" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Baldry", "given_name": "Ivan K.", "clpid": "Baldry-I-K" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" }, { "literal": "2dFGRS Team" } ], "abstract": "We have calculated the two-point correlation functions in redshift space, \u03be(\u03c3, \u03c0), for galaxies of different spectral types in the 2dF Galaxy Redshift Survey. Using these correlation functions, we are able to estimate values of the linear redshift-space distortion parameter, \u03b2\u2261\u03a9\u2070.\u2076\u03a9/b, the pairwise velocity dispersion, a, and the real-space correlation function, \u03be(r), for galaxies with both relatively low star formation rates (for which the present rate of star formation is less than 10 per cent of its past averaged value) and galaxies with higher current star formation activity. At small separations, the real-space clustering of passive galaxies is very much stronger than that of the more actively star-forming galaxies; the correlation-function slopes are, respectively, 1.93 and 1.50, and the relative bias between the two classes is a declining function of scale. On scales larger than 10 h\u207b\u00b9 Mpc, there is evidence that the relative bias tends to a constant, b_(passive)/b_(active) \u2243 1. This result is consistent with the similar degrees of redshift-space distortions seen in the correlation functions of the two classes \u2013 the contours of \u03be(\u03c3, \u03c0) require \u03b2_(active) = 0.49 \u00b1 0.13 and \u03b2_(passive) = 0.48 \u00b1 0.14. The pairwise velocity dispersion is highly correlated with \u03b2. Despite this, a significant difference is seen between the two classes. Over the range 8\u201320 h\u207b\u00b9 Mpc, the pairwise velocity dispersion has mean values of 416 \u00b1 76 and 612 \u00b1 92 km s\u207b\u00b9 for the active and passive galaxy samples, respectively. This is consistent with the expectation from morphological segregation, in which passively evolving galaxies preferentially inhabit the cores of high-mass virialized regions.", "doi": "10.1046/j.1365-8711.2003.06861.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2003-09-21", "series_number": "3", "volume": "344", "issue": "3", "pages": "847-856" }, { "id": "authors:4c8yr-zz578", "collection": "authors", "collection_id": "4c8yr-zz578", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200708-151732985", "type": "article", "title": "The 2dF Galaxy Redshift Survey: the luminosity function of cluster galaxies", "author": [ { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Baldry", "given_name": "Ivan K.", "clpid": "Baldry-I-K" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Cross", "given_name": "Nicholas", "clpid": "Cross-N-J-G" }, { "family_name": "Dalton", "given_name": "Gavin B.", "clpid": "Dalton-G-B" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Hawkins", "given_name": "Edward", "clpid": "Hawkins-E" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Madgwick", "given_name": "Darren S.", "clpid": "Madgwick-D-S" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Percival", "given_name": "Will", "clpid": "Percival-W-J" }, { "family_name": "Peterson", "given_name": "Bruce", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" } ], "abstract": "We have determined the composite luminosity function (LF) for galaxies in 60 clusters from the 2dF Galaxy Redshift Survey. The LF spans the range \u221222.5 < M_(bj) < \u221215, and is well fitted by a Schechter function with M\u2217_(bJ) = \u221220.07 \u00b1 0.07 and \u03b1 = \u22121.28 \u00b1 0.03 (H\u2080 = 100 km s\u207b\u00b9 Mpc\u207b\u00b9, \u03a9_M = 0.3, \u03a9_\u039b = 0.7). It differs significantly from the field LF, having a characteristic magnitude that is approximately 0.3 mag brighter and a faint-end slope that is approximately 0.1 steeper. There is no evidence for variations in the LF across a wide range of cluster properties: the LF is similar for clusters with high and low velocity dispersions, for rich and poor clusters, for clusters with different Bautz\u2013Morgan types, and for clusters with and without substructure. The core regions of clusters differ from the outer parts, however, in having an excess of very bright galaxies. We also construct the LFs for early (quiescent), intermediate and late (star-forming) spectral types. We find that, as in the field, the LFs of earlier-type galaxies have brighter characteristic magnitudes and shallower faint-end slopes. However, the LF of early-type galaxies in clusters is both brighter and steeper than its field counterpart, although the LF of late-type galaxies is very similar. The trend of faint-end slope with spectral type is therefore much less pronounced in clusters than in the field, explaining why variations in the mixture of types do not lead to significant differences in the cluster LFs. The differences between the field and cluster LFs for the various spectral types can be qualitatively explained by the suppression of star formation in the dense cluster environment, together with mergers to produce the brightest early-type galaxies.", "doi": "10.1046/j.1365-8711.2003.06510.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2003-07-01", "series_number": "3", "volume": "342", "issue": "3", "pages": "725-737" }, { "id": "authors:dwqe7-qcg77", "collection": "authors", "collection_id": "dwqe7-qcg77", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20150401-140640866", "type": "article", "title": "The bright optical afterglow of the nearby \u03b3-ray burst of 29 March 2003", "author": [ { "family_name": "Price", "given_name": "P. A.", "clpid": "Price-P-A" }, { "family_name": "Fox", "given_name": "D. W.", "orcid": "0000-0002-3714-672X", "clpid": "Fox-D-B" }, { "family_name": "Kulkarni", "given_name": "S. R.", "orcid": "0000-0001-5390-8563", "clpid": "Kulkarni-S-R" }, { "family_name": "Peterson", "given_name": "B. A.", "clpid": "Peterson-B-A" }, { "family_name": "Schmidt", "given_name": "B. P.", "orcid": "0000-0001-6589-1287", "clpid": "Schmidt-B-P" }, { "family_name": "Soderberg", "given_name": "A. M.", "clpid": "Soderberg-A-M" }, { "family_name": "Yost", "given_name": "S. A.", "clpid": "Yost-S-A" }, { "family_name": "Berger", "given_name": "E.", "orcid": "0000-0002-9392-9681", "clpid": "Berger-Edo" }, { "family_name": "Djorgovski", "given_name": "S. G.", "orcid": "0000-0002-0603-3087", "clpid": "Djorgovski-S-G" }, { "family_name": "Frail", "given_name": "D. A.", "clpid": "Frail-D-A" }, { "family_name": "Harrison", "given_name": "F. A.", "orcid": "0000-0002-4226-8959", "clpid": "Harrison-F-A" }, { "family_name": "Sari", "given_name": "R.", "orcid": "0000-0002-1084-3656", "clpid": "Sari-R" }, { "family_name": "Blain", "given_name": "A. W.", "orcid": "0000-0001-7489-5167", "clpid": "Blain-A-W" }, { "family_name": "Chapman", "given_name": "S. C.", "clpid": "Chapman-S-C" } ], "abstract": "Past studies of cosmological y-ray bursts (GRBs) have been hampered by their extreme distances, resulting in faint afterglows. A nearby GRB could potentially shed much light on the origin of these events, but GRBs with a redshift z \u2264 0.2 have been estimated to occur only rarely, about once per decade. Here we report the discovery of the bright optical afterglow emission from the burst of 29 March 2003 (GRB030329; ref. 2). The brightness of the afterglow and the prompt report of its position resulted in extensive follow-up observations at many wavelengths, along with the measurement of the redshift, z = 0.169 (ref. 4). The y-ray and afterglow properties of GRB030329 are similar to those of GRBs at cosmological redshifts. Observations have already identified the progenitor as a massive star that exploded as a supernova.", "doi": "10.1038/nature01734", "issn": "0028-0836", "publisher": "Nature Publishing Group", "publication": "Nature", "publication_date": "2003-06-19", "series_number": "6942", "volume": "423", "issue": "6942", "pages": "844-847" }, { "id": "authors:sgqhq-k0827", "collection": "authors", "collection_id": "sgqhq-k0827", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200629-094519270", "type": "article", "title": "Parameter constraints for flat cosmologies from cosmic microwave background and 2dFGRS power spectra", "author": [ { "family_name": "Percival", "given_name": "Will J.", "clpid": "Percival-W-J" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Moody", "given_name": "Stephen", "clpid": "Moody-Stephen" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" }, { "literal": "2dFGRS Team" } ], "abstract": "We constrain flat cosmological models with a joint likelihood analysis of a new compilation of data from the cosmic microwave background (CMB) and from the 2dF Galaxy Redshift Survey (2dFGRS). Fitting the CMB alone yields a known degeneracy between the Hubble constant h and the matter density \u03a9\u2098, which arises mainly from preserving the location of the peaks in the angular power spectrum. This 'horizon-angle degeneracy' is considered in some detail and is shown to follow the simple relation \u03a9\u2098h\u00b3.\u2074= constant. Adding the 2dFGRS power spectrum constrains \u03a9\u2098h and breaks the degeneracy. If tensor anisotropies are assumed to be negligible, we obtain values for the Hubble constant of h= 0.665 \u00b1 0.047, the matter density \u03a9\u2098 = 0.313 \u00b1 0.055, and the physical cold dark matter and baryon densities \u03a9ch\u00b2= 0.115 \u00b1 0.009, \u03a9bh\u00b2= 0.022 \u00b1 0.002 (standard rms errors). Including a possible tensor component causes very little change to these figures; we set an upper limit to the tensor-to-scalar ratio of r < 0.7 at a 95 per cent confidence level. We then show how these data can be used to constrain the equation of state of the vacuum, and find w < \u22120.52 at 95 per cent confidence. The preferred cosmological model is thus very well specified, and we discuss the precision with which future CMB data can be predicted, given the model assumptions. The 2dFGRS power-spectrum data and covariance matrix, and the CMB data compilation used here, are available from http://www.roe.ac.uk/\u223cwjp/.", "doi": "10.1046/j.1365-8711.2002.06001.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2002-12-11", "series_number": "3", "volume": "337", "issue": "3", "pages": "1068-1080" }, { "id": "authors:120nt-twp07", "collection": "authors", "collection_id": "120nt-twp07", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200708-151732795", "type": "article", "title": "The 2dF Galaxy Redshift Survey: the b_J-band galaxy luminosity function and survey selection function", "author": [ { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Baldry", "given_name": "Ivan", "clpid": "Baldry-I-K" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Cross", "given_name": "Nicholas J. G.", "clpid": "Cross-N-J-G" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Madgwick", "given_name": "Darren", "clpid": "Madgwick-D-S" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" }, { "literal": "2dFGRS Team" } ], "abstract": "We use more than 110 500 galaxies from the 2dF Galaxy Redshift Survey (2dFGRS) to estimate the b\u2c7c-band galaxy luminosity function at redshift z = 0, taking account of evolution, the distribution of magnitude measurement errors and small corrections for incompleteness in the galaxy catalogue. Throughout the interval \u221216.5 > M_(bJ) \u22125 log\u2081\u2080 h > \u221222, the luminosity function is accurately described by a Schechter function with M*_bJ \u22125 log\u2081\u2080 h = \u221219.66\u00b10.07, \u03b1 = \u22121.21\u00b10.03 and \u03a6* =(1.61\u00b10.08)\u00d710-\u00b2 h\u00b3 Mpc\u207b\u00b3, giving an integrated luminosity density of \u03c1L =(1.82\u00b10.17)\u00d710\u2078 h L_\u2299 Mpc\u207b\u00b3 (assuming an \u03a9\u2080 = 0.3, \u039b\u2080 = 0.7 cosmology). The quoted errors have contributions from the accuracy of the photometric zero-point, from large-scale structure in the galaxy distribution and, importantly, from the uncertainty in the appropriate evolutionary corrections. Our luminosity function is in excellent agreement with, but has much smaller statistical errors than, an estimate from the Sloan Digital Sky Survey (SDSS) data when the SDSS data are accurately translated to the b\u2c7c band and the luminosity functions are normalized in the same way. We use the luminosity function, along with maps describing the redshift completeness of the current 2dFGRS catalogue, and its weak dependence on apparent magnitude, to define a complete description of the 2dFGRS selection function. Details and tests of the calibration of the 2dFGRS photometric parent catalogue are also presented.", "doi": "10.1046/j.1365-8711.2002.05831.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2002-11-01", "series_number": "3", "volume": "336", "issue": "3", "pages": "907-931" }, { "id": "authors:a0kf5-99839", "collection": "authors", "collection_id": "a0kf5-99839", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20170408-195911451", "type": "article", "title": "The 2dF Galaxy Redshift Survey: the environmental dependence of galaxy star formation rates near clusters", "author": [ { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Balogh", "given_name": "Michael", "clpid": "Balogh-M-L" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Bower", "given_name": "Richard", "clpid": "Bower-R-G" }, { "family_name": "Offer", "given_name": "Allison", "clpid": "Offer-A" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Baldry", "given_name": "Ivan K.", "clpid": "Baldry-I-K" }, { "family_name": "Baugh", "given_name": "Carlton", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-T" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Cross", "given_name": "Nicholas", "clpid": "Cross-N-J-G" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Hawkins", "given_name": "Edward", "clpid": "Hawkins-E" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S" }, { "family_name": "Madgwick", "given_name": "Darren", "clpid": "Madgwick-D" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Percival", "given_name": "Will", "clpid": "Percival-W-J" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-K" } ], "abstract": "We have measured the equivalent width of the H\u03b1 emission line for 11 006 galaxies brighter than M_b-=-\u221219 (\u03a9_\u039b = 0.7, \u03a9_m = 0.3, H_0 = 70 km s^(\u22121) Mpc^(\u22121)) at 0.05 < z < 0.1 in the 2dF Galaxy Redshift Survey (2dFGRS), in the fields of 17 known galaxy clusters. The limited redshift range ensures that our results are insensitive to aperture bias, and to residuals from night sky emission lines. We use these measurements to trace \u03bc*, the star formation rate normalized to L*, as a function of distance from the cluster centre, and local projected galaxy density. We find that the distribution of \u03bc* steadily skews toward larger values with increasing distance from the cluster centre, converging to the field distribution at distances greater than \u223c3 times the virial radius. A correlation between star formation rate and local projected density is also found, which is independent of cluster velocity dispersion and disappears at projected densities below \u223c1 galaxy Mpc^(\u22122) (brighter than M_b = \u221219). This characteristic scale corresponds approximately to the mean density at the cluster virial radius. The same correlation holds for galaxies more than two virial radii from the cluster centre. We conclude that environmental influences on galaxy properties are not restricted to cluster cores, but are effective in all groups where the density exceeds this critical value. The present-day abundance of such systems, and the strong evolution of this abundance, makes it likely that hierarchical growth of structure plays a significant role in decreasing the global average star formation rate. Finally, the low star formation rates well beyond the virialized cluster rule out severe physical processes, such as ram pressure stripping of disc gas, as being completely responsible for the variations in galaxy properties with environment.", "doi": "10.1046/j.1365-8711.2002.05558.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2002-08-12", "series_number": "3", "volume": "334", "issue": "3", "pages": "673-683" }, { "id": "authors:p7st8-cyd38", "collection": "authors", "collection_id": "p7st8-cyd38", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200521-160221140", "type": "article", "title": "The 2dF Galaxy Redshift Survey: the population of nearby radio galaxies at the 1-mJy level", "author": [ { "family_name": "Magliocchetti", "given_name": "Manuela", "clpid": "Magliocchetti-M" }, { "family_name": "Maddox", "given_name": "Steve J.", "clpid": "Maddox-S-J" }, { "family_name": "Jackson", "given_name": "Carole A.", "clpid": "Jackson-C-A" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" } ], "abstract": "We use redshift determinations and spectral analysis of galaxies in the 2dF Galaxy Redshift Survey to study the properties of local radio sources with S \u22651 mJy. 557 objects (hereafter called the spectroscopic sample) drawn from the FIRST survey, corresponding to 2.3 per cent of the total radio sample, are found in the 2dFGRS catalogue within the area 9\u02b048\u1d50 \u2272 RA(2000) \u2272 14\u02b032\u1d50 and -2\u00b0.77 \u2272 Dec.(2000) \u2272 2\u00b0.25, down to a magnitude limit b_J = 19.45. The excellent quality of 2dF spectra allows us to divide these sources into classes, according to their optical spectra. \n\nAbsorption-line systems make up 63 per cent of the spectroscopic sample. These may or may not show emission lines due to AGN activity, and correspond to 'classical' radio galaxies belonging mainly to the FRI class. They are characterized by relatively high radio-to-optical ratios, red colours, and high radio luminosities (10\u00b2\u00b9 \u2272 P_(1.4 GHz)/W Hz\u207b\u00b9 sr\u207b\u00b9 \u2272 10\u00b2\u2074). Actively star-forming galaxies contribute about 32 per cent of the sample. These objects are mainly found at low redshifts (z \u2272 0.1) and show low radio-to-optical ratios, blue colours and low radio luminosities. We also found 18 Seyfert 2 galaxies (3 per cent) and four Seyfert 1s (1 per cent). \n\nAnalysis of the local radio luminosity function (LF) shows that radio galaxies are well described by models that assume pure luminosity evolution, at least down to radio powers P_(1.4 GHz) \u2272 10^(20.5) W Hz\u207b\u00b9 sr\u207b\u00b9. Late-type galaxies, whose relative contribution to the radio LF is found to be lower than was predicted by previous works, present an LF which is comparable with the IRAS galaxy LF. This class of sources therefore plausibly constitutes the radio counterpart of the dusty spirals and starbursts that dominate the counts at 60 \u03bcm.", "doi": "10.1046/j.1365-8711.2002.05386.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2002-06", "series_number": "1", "volume": "333", "issue": "1", "pages": "100-120" }, { "id": "authors:8p6e9-2ed45", "collection": "authors", "collection_id": "8p6e9-2ed45", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200610-122805395", "type": "article", "title": "The 2dF galaxy redshift survey: near-infrared galaxy luminosity functions", "author": [ { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Cross", "given_name": "Nicholas", "clpid": "Cross-N-J-G" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Madgwick", "given_name": "Darren", "clpid": "Madgwick-D-S" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" }, { "literal": "2dFGRS Team" } ], "abstract": "We combine the Two Micron All Sky Survey (2MASS) Extended Source Catalogue and the 2dF Galaxy Redshift Survey to produce an infrared selected galaxy catalogue with 17 173 measured redshifts. We use this extensive data set to estimate the galaxy luminosity functions in the J- and K_S-bands. The luminosity functions are fairly well fitted by Schechter functions with parameters M_J*\u22125 log h = \u221222.36\u00b10.02, \u03b1_J* = \u22120.93\u00b10.04, \u03a6_J* = 0.0104\u00b10.0016 h\u00b3 Mpc\u207b\u00b3 in the J-band and MK_S*\u22125 log h = \u221223.44\u00b10.03, \u03b1K_S = \u22120.96\u00b10.05, \u03a6K_S* = 0.0108\u00b10.0016 h\u00b3 Mpc\u207b\u00b3 in the K_S-band (2MASS Kron magnitudes). These parameters are derived assuming a cosmological model with \u03a9\u2080 = 0.3 and \u039b\u2080 = 0.7. With data sets of this size, systematic rather than random errors are the dominant source of uncertainty in the determination of the luminosity function. We carry out a careful investigation of possible systematic effects in our data. The surface brightness distribution of the sample shows no evidence that significant numbers of low surface brightness or compact galaxies are missed by the survey. We estimate the present-day distributions of b_J \u2014 K_S and J \u2014 K_S colours as a function of the absolute magnitude and use models of the galaxy stellar populations, constrained by the observed optical and infrared colours, to infer the galaxy stellar mass function. Integrated over all galaxy masses, this yields a total mass fraction in stars (in units of the critical mass density) of \u03a9_(stars)h = (1.6\u00b10.24) \u00d7 10\u207b\u00b3 for a Kennicutt initial mass function (IMF) and \u03a9_(stars)h = (2.9\u00b10.43) \u00d7 10\u207b\u00b3 for a Salpeter IMF. These values are consistent with those inferred from observational estimates of the total star formation history of the Universe provided that dust extinction corrections are modest.", "doi": "10.1046/j.1365-8711.2001.04591.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2001-09-01", "series_number": "1", "volume": "326", "issue": "1", "pages": "255-273" }, { "id": "authors:5b9p5-9cm21", "collection": "authors", "collection_id": "5b9p5-9cm21", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200629-094519018", "type": "article", "title": "The 2dF Galaxy Redshift Survey: the number and luminosity density of galaxies", "author": [ { "family_name": "Cross", "given_name": "Nicholas", "clpid": "Cross-N-J-G" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Baugh", "given_name": "Carlton M.", "orcid": "0000-0002-9935-9755", "clpid": "Baugh-C-M" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Bridges", "given_name": "Terry", "clpid": "Bridges-Terry" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "Deeley", "given_name": "Kathryn", "clpid": "Deeley-K" }, { "family_name": "De Propris", "given_name": "Roberto", "clpid": "De-Propris-R" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Jackson", "given_name": "Carole", "clpid": "Jackson-C-A" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Madgwick", "given_name": "Darren", "clpid": "Madgwick-D-S" }, { "family_name": "Moody", "given_name": "Stephen", "clpid": "Moody-S" }, { "family_name": "Norberg", "given_name": "Peder", "orcid": "0000-0002-5875-0440", "clpid": "Norberg-P" }, { "family_name": "Peacock", "given_name": "John A.", "clpid": "Peacock-J-A" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Price", "given_name": "Ian", "clpid": "Price-I" }, { "family_name": "Seaborne", "given_name": "Mark", "clpid": "Seaborne-M" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Tadros", "given_name": "Helen", "clpid": "Tadros-H" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" } ], "abstract": "We present the bivariate brightness distribution (BBD) for the 2dF Galaxy Redshift Survey (2dFGRS) based on a preliminary subsample of 45 000 galaxies. The BBD is an extension of the galaxy luminosity function, incorporating surface brightness information. It allows the measurement of the local luminosity density, j\u0299, and of the galaxy luminosity and surface brightness distributions, while accounting for surface brightness selection biases. \n\nThe recovered 2dFGRS BBD shows a strong luminosity\u2013surface brightness relation M\u0299\u221d(2.4\u00b1\u2080.\u2085\u00b9.\u2075)\u03bc\u2091], providing a new constraint for galaxy formation models. In terms of the number density, we find that the peak of the galaxy population lies at M\u0299\u2265\u221216.0 mag. Within the well-defined selection limits (\u221224", "doi": "10.1046/j.1365-8711.2001.04254.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "2001-07-01", "series_number": "4", "volume": "324", "issue": "4", "pages": "825-841" }, { "id": "authors:tykfb-5gt74", "collection": "authors", "collection_id": "tykfb-5gt74", "cite_using_url": "https://resolver.caltech.edu/CaltechAUTHORS:20200629-094518760", "type": "article", "title": "The 2dF Galaxy Redshift Survey: spectral types and luminosity functions", "author": [ { "family_name": "Folkes", "given_name": "Simon", "clpid": "Folkes-S" }, { "family_name": "Ronen", "given_name": "Shai", "clpid": "Ronen-S" }, { "family_name": "Price", "given_name": "Ian", "clpid": "Price-I" }, { "family_name": "Lahav", "given_name": "Ofer", "clpid": "Lahav-O" }, { "family_name": "Colless", "given_name": "Matthew", "orcid": "0000-0001-9552-8075", "clpid": "Colless-M" }, { "family_name": "Maddox", "given_name": "Steve", "clpid": "Maddox-S-J" }, { "family_name": "Deeley", "given_name": "Kathryn", "clpid": "Deeley-K" }, { "family_name": "Glazebrook", "given_name": "Karl", "clpid": "Glazebrook-K" }, { "family_name": "Bland-Hawthorn", "given_name": "Joss", "orcid": "0000-0001-7516-4016", "clpid": "Bland-Hawthorn-J" }, { "family_name": "Cannon", "given_name": "Russell", "clpid": "Cannon-R" }, { "family_name": "Cole", "given_name": "Shaun", "clpid": "Cole-S" }, { "family_name": "Collins", "given_name": "Chris", "clpid": "Collins-C-A" }, { "family_name": "Couch", "given_name": "Warrick", "clpid": "Couch-W-J" }, { "family_name": "Driver", "given_name": "Simon P.", "clpid": "Driver-S-P" }, { "family_name": "Dalton", "given_name": "Gavin", "clpid": "Dalton-G" }, { "family_name": "Efstathiou", "given_name": "George", "clpid": "Efstathiou-G" }, { "family_name": "Ellis", "given_name": "Richard S.", "orcid": "0000-0001-7782-7071", "clpid": "Ellis-R-S" }, { "family_name": "Frenk", "given_name": "Carlos S.", "clpid": "Frenk-C-S" }, { "family_name": "Kaiser", "given_name": "Nick", "orcid": "0000-0001-6511-4306", "clpid": "Kaiser-N" }, { "family_name": "Lewis", "given_name": "Ian", "clpid": "Lewis-I-A" }, { "family_name": "Lumsden", "given_name": "Stuart", "clpid": "Lumsden-S" }, { "family_name": "Peacock", "given_name": "John", "clpid": "Peacock-J-A" }, { "family_name": "Peterson", "given_name": "Bruce A.", "clpid": "Peterson-B-A" }, { "family_name": "Sutherland", "given_name": "Will", "clpid": "Sutherland-W" }, { "family_name": "Taylor", "given_name": "Keith", "clpid": "Taylor-Keith" } ], "abstract": "We describe the 2dF Galaxy Redshift Survey (2dFGRS) and the current status of the observations. In this exploratory paper, we apply a principal component analysis to a preliminary sample of 5869 galaxy spectra and use the two most significant components to split the sample into five spectral classes. These classes are defined by considering visual classifications of a subset of the 2dF spectra, and also by comparison with high-quality spectra of local galaxies. We calculate a luminosity function for each of the different classes and find that later-type galaxies have a fainter characteristic magnitude, and a steeper faint-end slope. For the whole sample we find M*=\u221219.7 (for \u03a9=1, H\u2080=100 km s\u207b\u00b9 Mpc\u207b\u00b9), \u03b1=\u22121.3, \u03c6*=0.017. For class 1 ('early-type') we find M*=\u221219.6, \u03b1=\u22120.7, while for class 5 ('late-type') we find M*=\u221219.0, \u03b1=\u22121.7. The derived 2dF luminosity functions agree well with other recent luminosity function estimates.", "doi": "10.1046/j.1365-8711.1999.02721.x", "issn": "0035-8711", "publisher": "Royal Astronomical Society", "publication": "Monthly Notices of the Royal Astronomical Society", "publication_date": "1999-09-19", "series_number": "2", "volume": "308", "issue": "2", "pages": "459-472" } ]