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Ariel G. Sanchez,
C. G. Scoccola,
A. J. Ross,
W. Percival,
M. Manera,
F. Montesano,
X. Mazzalay,
A. J. Cuesta, D. J. Eisenstein,
E. Kazin, [......],
R. Skibba,
S. Snedden,
D. Thomas,
J. Tinker,
D. A. Wake,
B. A. Weaver,
David H. Weinberg,
Martin White,
I. Zehavi,
G. Zhao
[show abstract]
[hide abstract]
ABSTRACT: We obtain constraints on cosmological parameters from the spherically
averaged redshift-space correlation function of the CMASS Data Release 9 (DR9)
sample of the Baryonic Oscillation Spectroscopic Survey (BOSS). We combine this
information with additional data from recent CMB, SN and BAO measurements. Our
results show no significant evidence of deviations from the standard
flat-Lambda CDM model, whose basic parameters can be specified by Omega_m =
0.285 +- 0.009, 100 Omega_b = 4.59 +- 0.09, n_s = 0.96 +- 0.009, H_0 = 69.4 +-
0.8 km/s/Mpc and sigma_8 = 0.80 +- 0.02. The CMB+CMASS combination sets tight
constraints on the curvature of the Universe, with Omega_k = -0.0043 +- 0.0049,
and the tensor-to-scalar amplitude ratio, for which we find r < 0.16 at the 95
per cent confidence level (CL). These data show a clear signature of a
deviation from scale-invariance also in the presence of tensor modes, with n_s
<1 at the 99.7 per cent CL. We derive constraints on the fraction of massive
neutrinos of f_nu < 0.049 (95 per cent CL), implying a limit of sum m_nu < 0.51
eV. We find no signature of a deviation from a cosmological constant from the
combination of all datasets, with a constraint of w_DE = -1.033 +- 0.073 when
this parameter is assumed time-independent, and no evidence of a departure from
this value when it is allowed to evolve as w_DE(a) = w_0 + w_a (1 - a). The
achieved accuracy on our cosmological constraints is a clear demonstration of
the constraining power of current cosmological observations.
03/2012;
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C. S. Kochanek, D. J. Eisenstein,
R. J. Cool,
N. Caldwell,
R. J. Assef,
B. T. Jannuzi,
C Jones,
S. S. Murray,
W. R. Forman,
A. Dey,
M. J. I. Brown,
P. Eisenhardt,
A. H. Gonzalez,
P. Green,
D. Stern
[show abstract]
[hide abstract]
ABSTRACT: The AGN and Galaxy Evolution Survey (AGES) is a redshift survey covering, in
its standard fields, 7.7 square degrees of the Bootes field of the NOAO Deep
Wide-Field Survey (NDWFS). The final sample consists of 23745 redshifts. There
are well-defined galaxy samples in ten bands (the Bw, R, I, J, K, IRAC 3.6,
4.5, 5.8 and 8.0 micron and MIPS 24 micron bands) to a limiting magnitude of
I<20 mag for spectroscopy. For these galaxies, we obtained 18163 redshifts from
a sample of 35200 galaxies, where random sparse sampling was used to define
statistically complete sub-samples in all ten photometric bands. The median
galaxy redshift is 0.31, and 90% of the redshifts are in the range
0.085<z<0.66. AGN were selected as radio, X-ray, IRAC mid-IR and MIPS 24 micron
sources to fainter limiting magnitudes (I<22.5 mag for point sources).
Redshifts were obtained for 4764 quasars and galaxies with AGN signatures, with
2926, 1718, 605, 119 and 13 above redshifts of 0.5, 1, 2, 3 and 4,
respectively. We detail all the AGES selection procedures and present the
complete spectroscopic redshift catalogs, spectra, and spectral energy
distribution decompositions. The photometric redshift estimates are for all
sources in the AGES samples.
10/2011;
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H Aihara,
C Allende Prieto,
D An,
S ~F Anderson,
É Aubourg,
E Balbinot,
T ~C Beers,
A ~A Berlind,
S ~J Bickerton,
D Bizyaev, [......],
D ~A Wake,
J Wang,
B ~A Weaver,
D ~H Weinberg,
M White,
S ~D ~M White,
B Yanny,
N Yasuda,
C Yeche,
I Zehavi
apjs. 08/2011; 195:26.
-
H Aihara,
C Allende Prieto,
D An,
S ~F Anderson,
É Aubourg,
E Balbinot,
T ~C Beers,
A ~A Berlind,
S ~J Bickerton,
D Bizyaev, [......],
D ~A Wake,
J Wang,
B ~A Weaver,
D ~H Weinberg,
M White,
S ~D ~M White,
B Yanny,
N Yasuda,
C Yeche,
I Zehavi
apjs. 08/2011; 195:26.
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T. Matheson,
P. M. Garnavich,
K. Z. Stanek,
D. Bersier,
S. T. Holland,
K. Krisciunas,
N. Caldwell,
P. Berlind,
J. S. Bloom,
M. Bolte, [......],
B. Pindor,
D. D. Sasselov,
R. Schild,
H. Schweiker,
T. Spahr,
J. Thomas-Osip,
I. Thompson,
D. Weisz,
R. Windhorst,
and D. Zaritsky
[show abstract]
[hide abstract]
ABSTRACT: We present extensive optical and infrared photometry of the afterglow of gamma-ray burst (GRB) 030329 and its associated supernova (SN) 2003dh over the first two months after detection (2003 March 30-May 29 UT). Optical spectroscopy from a variety of telescopes is shown and, when combined with the photometry, allows an unambiguous separation between the afterglow and SN contributions. The optical afterglow of the GRB is initially a power-law continuum but shows significant color variations during the first week that are unrelated to the presence of an SN. The early afterglow light curve also shows deviations from the typical power-law decay. An SN spectrum is first detectable ~7 days after the burst and dominates the light after ~11 days. The spectral evolution and the light curve are shown to closely resemble those of SN 1998bw, a peculiar Type Ic SN associated with GRB 980425, and the time of the SN explosion is close to the observed time of the GRB. It is now clear that at least some GRBs arise from core-collapse SNe.
The Astrophysical Journal 12/2008; 599(1):394. · 6.02 Impact Factor
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[show abstract]
[hide abstract]
ABSTRACT: We report the discovery of 11 new variable DA white dwarf (ZZ Ceti) stars. Candidates were selected by deriving temperatures from model fits to spectra obtained from the Sloan Digital Sky Survey (SDSS). We also find objects whose temperatures and gravities indicate they lie within the instability strip for pulsation but were not observed to vary. Although the temperatures are based on relatively low signal-to-noise ratio spectra, an impure strip is unexpected, which if confirmed, has implications for DA asteroseismology. This work brings the total number of published variable DA white dwarf stars to 82.
The Astrophysical Journal 12/2008; 625(2):966. · 6.02 Impact Factor
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K. Z. Stanek,
T. Matheson,
P. M. Garnavich,
P. Martini,
P. Berlind,
N. Caldwell,
P. Challis,
W. R. Brown,
R. Schild,
K. Krisciunas, [......],
N. Hathi,
R. A. Jansen,
R. Windhorst,
L. Echevarria, D. J. Eisenstein,
B. Pindor,
E. W. Olszewski,
P. Harding,
S. T. Holland,
and D. Bersier
[show abstract]
[hide abstract]
ABSTRACT: We present early observations of the afterglow of GRB 030329 and the spectroscopic discovery of its associated supernova SN 2003dh. We obtained spectra of the afterglow of GRB 030329 each night from March 30.12 (0.6 days after the burst) to April 8.13 (UT) (9.6 days after the burst). The spectra cover a wavelength range of 350-850 nm. The early spectra consist of a power-law continuum (Fν ν-0.9) with narrow emission lines originating from H II regions in the host galaxy, indicating a low redshift of z = 0.1687. However, our spectra taken after 2003 April 5 show broad peaks in flux characteristic of a supernova. Correcting for the afterglow emission, we find that the spectrum of the supernova is remarkably similar to the Type Ic "hypernova" SN 1998bw. While the presence of supernovae has been inferred from the light curves and colors of gamma-ray burst afterglows in the past, this is the first direct, spectroscopic confirmation that a subset of classical gamma-ray bursts originate from supernovae.
The Astrophysical Journal 12/2008; 591(1):L17. · 6.02 Impact Factor
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M. Brodwin,
M. J. I. Brown,
M. L. N. Ashby,
C. Bian,
K. Brand,
A. Dey,
P. R. Eisenhardt, D. J. Eisenstein,
A. H. Gonzalez,
J S Huang,
B. T. Jannuzi,
C. S. Kochanek,
E. McKenzie,
M. A. Pahre,
H. A. Smith,
B. T. Soifer,
S. A. Stanford,
D. Stern,
R. J. Elston
[show abstract]
[hide abstract]
ABSTRACT: Accurate photometric redshifts are calculated for nearly 200,000 galaxies to a 4.5 micron flux limit of ~13 uJy in the 8.5 deg^2 Spitzer/IRAC Shallow survey. Using a hybrid photometric redshift algorithm incorporating both neural-net and template-fitting techniques, calibrated with over 15,000 spectroscopic redshifts, a redshift accuracy of \sigma = 0.06(1+z) is achieved for 95% of galaxies at 0<z<1.5. The accuracy is \sigma = 0.12(1+z) for 95% of AGN at 0<z<3. Redshift probability functions, central to several ongoing studies of the galaxy population, are computed for the full sample. We demonstrate that these functions accurately represent the true redshift probability density, allowing the calculation of valid confidence intervals for all objects. These probability functions have already been used to successfully identify a population of Spitzer-selected high redshift (z>1) galaxy clusters. We present one such spectroscopically confirmed cluster at =1.24, ISCS J1434.5+3427. Finally, we present a measurement of the 4.5 micron-selected galaxy redshift distribution.
08/2006;
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D. A. Wake,
R. C. Nichol, D. J. Eisenstein,
J. Loveday,
A. C. Edge,
R. Cannon,
I. Smail,
D. P. Schneider,
Ryan Scranton,
D. Carson, [......],
J. da Angela,
S. Jester,
R. De Propris,
M. J. Drinkwater,
J. Bland-Hawthorn,
K. A. Pimbblet,
I. G. Roseboom,
T. Shanks,
R. G. Sharp,
J. Brinkmann
[show abstract]
[hide abstract]
ABSTRACT: We present new measurements of the luminosity function (LF) of Luminous Red Galaxies (LRGs) from the Sloan Digital Sky Survey (SDSS) and the 2dF-SDSS LRG and Quasar (2SLAQ) survey. We have carefully quantified, and corrected for, uncertainties in the K and evolutionary corrections, differences in the colour selection methods, and the effects of photometric errors, thus ensuring we are studying the same galaxy population in both surveys. Using a limited subset of 6326 SDSS LRGs (with 0.17<z<0.24) and 1725 2SLAQ LRGs (with 0.5 <z<0.6), for which the matching colour selection is most reliable, we find no evidence for any additional evolution in the LRG LF, over this redshift range, beyond that expected from a simple passive evolution model. This lack of additional evolution is quantified using the comoving luminosity density of SDSS and 2SLAQ LRGs, brighter than M_r - 5logh = -22.5, which are 2.51+/-0.03 x 10^-7 L_sun Mpc^-3 and 2.44+/-0.15 x 10^-7 L_sun Mpc^-3 respectively (<10% uncertainty). We compare our LFs to the COMBO-17 data and find excellent agreement over the same redshift range. Together, these surveys show no evidence for additional evolution (beyond passive) in the LF of LRGs brighter than M_r - 5logh = -21 (or brighter than L*). We test our SDSS and 2SLAQ LFs against a simple ``dry merger'' model for the evolution of massive red galaxies and find that at least half of the LRGs at z=0.2 must already have been well-assembled (with more than half their stellar mass) by z=0.6. This limit is barely consistent with recent results from semi-analytical models of galaxy evolution. Comment: Accepted for publication in MNRAS. 15 pages. See http://www.2slaq.info for further information
07/2006;
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M. Steinmetz,
T. Zwitter,
A. Siebert,
F. G. Watson,
K. C. Freeman,
U. Munari,
R Campbell,
M Williams,
G. M. Seabroke,
R. F. G. Wyse, [......],
G. Ruchti,
R. -D. Scholz,
A. Siviero,
M. C. Smith,
R. Sordo,
L. Veltz,
S. Vidrih,
R. von Berlepsch,
B. J. Boyle,
E. Schilbach
[show abstract]
[hide abstract]
ABSTRACT: We present the first data release of the Radial Velocity Experiment (RAVE), an ambitious spectroscopic survey to measure radial velocities and stellar atmosphere parameters (temperature, metallicity, surface gravity) of up to one million stars using the 6dF multi-object spectrograph on the 1.2-m UK Schmidt Telescope of the Anglo-Australian Observatory (AAO). The RAVE program started in 2003, obtaining medium resolution spectra (median R=7,500) in the Ca-triplet region ($\lambda\lambda$ 8,410--8,795 \AA) for southern hemisphere stars drawn from the Tycho-2 and SuperCOSMOS catalogs, in the magnitude range 9<I<12. The first data release is described in this paper and contains radial velocities for 24,748 individual stars (25,274 measurements when including re-observations). Those data were obtained on 67 nights between 11 April 2003 to 03 April 2004. The total sky coverage within this data release is $\sim$4,760 square degrees. The average signal to noise ratio of the observed spectra is 29.5, and 80% of the radial velocities have uncertainties better than 3.4 km/s. Combining internal errors and zero-point errors, the mode is found to be 2 km/s. Repeat observations are used to assess the stability of our radial velocity solution, resulting in a variance of 2.8 km/s. We demonstrate that the radial velocities derived for the first data set do not show any systematic trend with color or signal to noise. The RAVE radial velocities are complemented in the data release with proper motions from Starnet 2.0, Tycho-2 and SuperCOSMOS, in addition to photometric data from the major optical and infrared catalogs (Tycho-2, USNO-B, DENIS and 2MASS). The data release can be accessed via the RAVE webpage: http://www.rave-survey.org.
07/2006;
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B. G. Castanheira,
S. O. Kepler,
F. Mullally,
D. E. Winget,
D. Koester,
B. Voss,
S. J. Kleinman,
A. Nitta, D. J. Eisenstein,
R. Napiwotzki,
D. Reimers
[show abstract]
[hide abstract]
ABSTRACT: We report the discovery of eleven new ZZ Cetis using telescopes at OPD (Observat\'orio do Pico dos Dias/LNA) in Brazil, the 4.1 m SOAR (Southern Astrophysical Research) telescope at Cerro Pachon, Chile, and the 2.1 m Otto Struve telescope at McDonald observatory. The candidates were selected from the SDSS (Sloan Digital Sky Survey) and SPY (ESO SN Ia progenitor survey), based on their Teff obtained from optical spectra fitting. This selection criterion yields the highest success rate of detecting new ZZ Cetis, above 90% in the Teff range from 12000 to 11000 K. We also report on a DA not observed to vary, with a Teff placing the star close to the blue edge of the instability strip. Among our new pulsators, one is a little bit cooler than this star for which pulsations were not detected. Our observations are an important constraint on the location of the blue edge of the ZZ Ceti instability strip. Comment: 10 pages, 3 figures, to be published in A&A
11/2005;
-
[show abstract]
[hide abstract]
ABSTRACT: Baryonic acoustic oscillations imprinted in the galaxy power spectrum
provide a promising tool for probing dark energy. We present results
from a suite of cosmological N-body simulations aimed at investigating
possible systematic errors. We show the robustness of baryonic peaks
against nonlinearity, redshift distortions, and biases within the linear
region at various redshifts.
07/2005; 339:195.
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[show abstract]
[hide abstract]
ABSTRACT: We report the discovery of fourteen new ZZ Cetis with the 4.1m Southern Astrophysical Research telescope, at Cerro Pachon, in Chile. The candidates were selected from the SDSS (Sloan Digital Sky Survey) DA white dwarf stars with Teff obtained from the optical spectra fit, inside the ZZ Ceti instability strip. Considering these stars are multi-periodic pulsators and the pulsations propagate to the nucleus of the star, they carry information on the structure of the star and evolution of the progenitors. The ZZ Cetis discovered till 2003 are mainly within 100 pc from the Sun, and probe only the solar vicinity. The recently discovered ones, and those reported here, may sample a distinct population as they were selected mainly perpendicular to the galactic disk and cover a distance up to ~400pc. Comment: 12 pages, 2 figures
07/2005;
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D. P. Schneider,
P. B. Hall,
G. T. Richards,
D. E. Vanden Berk,
S. F. Anderson,
X Fan,
S. Jester,
C. Stoughton,
M. A. Strauss,
M. Subbarao, [......],
A. Nitta,
J. R. Pier,
C. M. Rockosi,
D. H. Saxe,
D. J. Schlegel,
S. A. Snedden,
A. S. Szalay,
A. R. Thakar,
A. Uomoto,
D. G. York
[show abstract]
[hide abstract]
ABSTRACT: We present the third edition of the Sloan Digital Sky Survey (SDSS) Quasar Catalog. The catalog consists of the 46,420 objects in the SDSS Third Data Release that have luminosities larger than M_i = -22 (in a cosmology with H_0 = 70 km/s/Mpc, Omega_M = 0.3, and Omega_Lambda = 0.7), have at least one emission line with FWHM larger than 1000 km/s or are unambiguously broad absorption line quasars, are fainter than i = 15.0, and have highly reliable redshifts. The area covered by the catalog is 4188 sq. deg. The quasar redshifts range from 0.08 to 5.41, with a median value of 1.47; the high-redshift sample includes 520 quasars at redshifts greater than four, of which 17 are at redshifts greater than five. For each object the catalog presents positions accurate to better than 0.2 arcsec. rms per coordinate, five-band (ugriz) CCD-based photometry with typical accuracy of 0.03 mag, and information on the morphology and selection method. The catalog also contains radio, near-infrared, and X-ray emission properties of the quasars, when available, from other large-area surveys. The calibrated digital spectra cover the wavelength region 3800--9200A at a spectral resolution about 2000; the spectra can be retrieved from the public database using the information provided in the catalog. A total of 44,221 objects in the catalog were discovered by the SDSS; 28,400 of the SDSS discoveries are reported here for the first time.
04/2005;
-
[show abstract]
[hide abstract]
ABSTRACT: The IRAC Shallow Survey is an 8.5 deg2 mid-IR imaging survey
in the NDWFS Bootes field. Combining the optical and infrared data
reliable photometric redshifts can be computed for hundreds of thousands
of IRAC-selected galaxies to z ˜ 1.5 with an accuracy of σ
z/(1+z) ˜ 0.07. This sample is ideal for studies of the
redshift evolution of the clustered galaxy population, both in the field
and in clusters of galaxies. An update of an ongoing high redshift (1
< z < 2) galaxy cluster search will be given, along with
preliminary measurements of the two-point correlation function of field
galaxies.
04/2005; 37:459.
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[show abstract]
[hide abstract]
ABSTRACT: We report the discovery of eleven new variable DA white dwarf (ZZ Ceti) stars. Candidates were selected by deriving temperatures from model fits to spectra obtained from the Sloan Digital Sky Survey. We also find objects whose temperatures and gravities indicate they lie within the instability strip for pulsation, but which were not observed to vary. Although the temperatures are based on relatively low S/N spectra, an impure strip is unexpected, and if confirmed suggests that our knowledge of the pulsation mechanism is incomplete. This work brings the total number of published variable DA white dwarf stars to 82.
03/2005;
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I. K. Baldry,
K. Glazebrook,
T. Budavári, D. J. Eisenstein,
J. Annis,
N. A. Bahcall,
M. R. Blanton,
J. Brinkmann,
I. Csabai,
T. M. Heckman,
H. Lin,
J. Loveday,
R. C. Nichol,
D. P. Schneider
[show abstract]
[hide abstract]
ABSTRACT: We construct and analyse a u-band selected galaxy sample from the Sloan Digital Sky Survey (SDSS) Southern Survey, which covers 275 deg2. The sample includes 43 223 galaxies with spectroscopic redshifts in the range 0.005 < z < 0.3 and with 14.5 < u < 20.5. The signal-to-noise (S/N) ratio in the u-band Petrosian aperture is improved by co-adding multiple epochs of imaging data and by including sky-subtraction corrections. Luminosity functions for the near-UV 0.1u band (λ≈ 322 ± 26 nm) are determined in redshift slices of width 0.02, which show a highly significant evolution in M* of −0.8 ± 0.1 mag between z= 0 and 0.3; with M*−5 log h70=−18.84 ± 0.05 (AB mag), log φ*=−2.06 ± 0.03 (h370 Mpc−3) and log ρL= 19.11 ± 0.02 (h70 W Hz−1 Mpc−3) at z= 0.1. The faint-end slope determined for z < 0.06 is given by α=−1.05 ± 0.08. This is in agreement with recent determinations from the Galaxy Evolution Explorer at shorter wavelengths. Comparing our z < 0.3 luminosity density measurements with 0.2 < z < 1.2 from Classifying Objects by Medium Band Observations in 17 Filters (COMBO-17), we find that the 280-nm density evolves as ρL∝ (1 +z)β with β= 2.1 ± 0.2; and find no evidence for any change in slope over this redshift range. By comparing with other measurements of cosmic star formation history, we estimate that the effective dust attenuation at 280 nm has increased by 0.8 ± 0.3 mag between z= 0 and 1.
Monthly Notices of the Royal Astronomical Society 03/2005; 358(2):441 - 456. · 4.90 Impact Factor
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D. J. Eisenstein,
I. Zehavi,
D. W. Hogg,
R. Scoccimarro,
M. R. Blanton,
R. C. Nichol,
R. Scranton,
H Seo,
M. Tegmark,
Z. Zheng, [......],
D Schneider,
K. Shimasaku,
C. Stoughton,
M Strauss,
M. Subbarao,
A. S. Szalay,
I. Szapudi,
D. Tucker,
B. Yanny,
D. York
[show abstract]
[hide abstract]
ABSTRACT: We present the large-scale correlation function measured from a spectroscopic sample of 46,748 luminous red galaxies from the Sloan Digital Sky Survey. The survey region covers 0.72 h^{-3} Gpc^3 over 3816 square degrees and 0.16<z<0.47, making it the best sample yet for the study of large-scale structure. We find a well-detected peak in the correlation function at 100h^{-1} Mpc separation that is an excellent match to the predicted shape and location of the imprint of the recombination-epoch acoustic oscillations on the low-redshift clustering of matter. This detection demonstrates the linear growth of structure by gravitational instability between z=1000 and the present and confirms a firm prediction of the standard cosmological theory. The acoustic peak provides a standard ruler by which we can measure the ratio of the distances to z=0.35 and z=1089 to 4% fractional accuracy and the absolute distance to z=0.35 to 5% accuracy. From the overall shape of the correlation function, we measure the matter density Omega_mh^2 to 8% and find agreement with the value from cosmic microwave background (CMB) anisotropies. Independent of the constraints provided by the CMB acoustic scale, we find Omega_m = 0.273 +- 0.025 + 0.123 (1+w_0) + 0.137 Omega_K. Including the CMB acoustic scale, we find that the spatial curvature is Omega_K=-0.010+-0.009 if the dark energy is a cosmological constant. More generally, our results provide a measurement of cosmological distance, and hence an argument for dark energy, based on a geometric method with the same simple physics as the microwave background anisotropies. The standard cosmological model convincingly passes these new and robust tests of its fundamental properties.
02/2005;
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I. K. Baldry,
K. Glazebrook,
T. Budavari, D. J. Eisenstein,
J. Annis,
N. A. Bahcall,
M. R. Blanton,
J. Brinkmann,
I. Csabai,
T. M. Heckman,
H Lin,
J. Loveday,
R. C. Nichol,
D. P. Schneider
[show abstract]
[hide abstract]
ABSTRACT: We construct and analyze a u-band selected galaxy sample from the SDSS Southern Survey, which covers 275 sq. deg. The sample includes 43223 galaxies with spectroscopic redshifts in the range 0.005<z<0.3 and with 14.5<u<20.5. The S/N in the u-band Petrosian aperture is improved by coadding multiple epochs of imaging data and by including sky-subtraction corrections. Luminosity functions for the near-UV ^{0.1}u band (322+-26 nm) are determined in redshift slices of width 0.02, which show a highly significant evolution in M^{star} of -0.8+-0.1 mag between z=0 and 0.3; with M^{star} = -18.84+-0.05 (AB mag), log phi^{star} = -2.06+-0.03 (Mpc^{-3}) and log rho_L = 19.11+-0.02 (W Hz^{-1} Mpc^{-3}) at z=0.1. The faint-end slope determined for z<0.06 is given by alpha=-1.05+-0.08. This is in agreement with recent determinations from GALEX at shorter wavelengths. Comparing our z<0.3 luminosity density measurements with 0.2<z<1.2 from COMBO-17, we find that the 280-nm density evolves as rho_L proportional to (1+z)^{beta} with beta=2.1+-0.2; and find no evidence for any change in slope over this redshift range. By comparing with other measurements of cosmic star formation history, we estimate that the effective dust attenuation at 280 nm has increased by 0.8+-0.3 mag between z=0 and 1. Comment: 18 pages, 17 figures, accepted by MNRAS (13 pages, 12 figures, excluding Appendices)
01/2005;
-
[show abstract]
[hide abstract]
ABSTRACT: Using the Karhunen-Loeve transform we present new results on the large
scale clustering of galaxies in the SDSS redshift sample.The likelihood
analysis of the cosmological parameters and those of the fluctuation
spectrum are all in excellent agreement with recent CMB results.
Proceedings of the International Astronomical Union 12/2004; 216:129.
