New Insight on Galaxy Formation and Evolution From Keck Spectroscopy of the Hawaii Deep Fields

Cowie, L. L.; Songaila, A.; Hu, E. M.; Cohen, Judith G.

doi:10.1086/118058

Cited by 1,623 publications

(1,851 citation statements)

References 32 publications

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“…The total number of redshifts is about 590, and the sample is 90% complete down to I ¼ 23. This limit is about 1.5 mag fainter than that of 4 m class surveys (e.g., CFRS) and comparable to other Keck telescope faint-galaxy surveys Cowie et al 1996).…”

Section: Spectroscopic Datasupporting

confidence: 63%

“…An L Ã early-type galaxy (M B ' À19:4 þ 5 log h; Marzke et al 1998) would have an apparent magnitude of I ' 20-21 at z ' 1, depending on the details of its luminosity evolution. Currently, the determination of redshifts of I $ 22 early-type galaxies is feasible with ground-based telescopes of aperture e4 m (Koo et al 1996;Lilly et al 1995;Cowie et al 1996;Cohen et al 1996Cohen et al , 2000. Moreover, previous studies have shown that morphological classification of faint galaxies is possible down to I ' 22:5 using Hubble Space Telescope (HST) images with exposure times e1 hr (Griffiths et al 1994a(Griffiths et al , 1994bDriver, Windhorst, & Griffiths 1995;Glazebrook et al 1995;Im et al 1996Im et al , 1995aAbraham et al 1996;Brinchmann et al 1998;Schade et al 1999;Im, Griffiths, & Ratnatunga 2000;Roche et al 1996Roche et al , 1998.…”

Section: Introductionmentioning

confidence: 99%

See 1 more Smart Citation

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

132

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We present the luminosity function and color-redshift relation of a magnitude-limited sample of 145 mostly red field E/S0 galaxies at zd1 from the DEEP Groth Strip Survey (GSS). Using nearby galaxy images as a training set, we develop a quantitative method to classify E/S0 galaxies based on smoothness, symmetry, and bulge-to-total light ratio. Using this method, we identify 145 E/S0's at 16:5 < I < 22 within the GSS, for which 44 spectroscopic redshifts (z spec ) are available. Most of the galaxies with spectroscopic redshifts (86%) form a '' red envelope '' in the redshift-color diagram, consistent with predictions of spectral synthesis models in which the dominant stellar population is formed at redshifts ze1:5. We use the tight correlation between VÀI and z spec for this red subset to estimate redshifts of the remaining E/S0's to an accuracy of $10%, with the exception of a small number (16%) of blue interlopers at low redshift that are quantitatively classified as E/S0's but are not contained within the red envelope. Constructing a luminosity function of the full sample of 145 E/S0's, we find that there is about 1.1-1.9 mag brightening in rest-frame B-band luminosity back to z ' 0:8 from z ¼ 0, consistent with other studies. Together with the red colors, this brightening is consistent with models in which the bulk of stars in red field E/S0's formed before z for e1:5 and have been evolving rather quiescently, with few large starbursts since then. Evolution in the number density of field E/ S0 galaxies is more difficult to measure, and uncertainties in the raw counts and their ratio to local samples might amount to as much as a factor of 2. Within that uncertainty, the number density of red E/S0's to z ' 0:8 seems relatively static, being comparable to or perhaps moderately less than that of local E/S0's, depending on the assumed cosmology. A doubling of E/S0 number density since z ¼ 1 can be ruled out with high confidence (97%) if m ¼ 1. Taken together, our results are consistent with the hypothesis that the majority of luminous field E/S0's were already in place by z $ 1, that the bulk of their stars were already fairly old, and that their number density has not changed by large amounts since then.

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Section: Spectroscopic Datasupporting

confidence: 63%

Section: Introductionmentioning

confidence: 99%

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Simard

Faber

et al. 2002

ApJ

142

132

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“…The shaded areas, at 0 < z < 0.5 and 3.5 < z < 6.4 highlight redshift space where log(L IR )≈ 12.5 galaxies are perceived to be rare. At 0 < z < 0.5 this is because they have a very low volume density, attributable to cosmic downsizing (Cowie et al, 1996), whereas at high-redshift (3.5 < z < 6.4) it is unknown whether or not the volume density of DSFGs is much lower since galaxies are much more difficult to spectroscopically confirm. At present, no purely star-forming DSFG at redshifts above z ≈ 6.4 has been discovered.…”

Section: The Very Negative K-correctionmentioning

confidence: 99%

Dusty star-forming galaxies at high redshift

2014

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Far-infrared and submillimeter wavelength surveys have now established the important role of dusty, star-forming galaxies (DSFGs) in the assembly of stellar mass and the evolution of massive galaxies in the Universe. The brightest of these galaxies have infrared luminosities in excess of 10 13 L with implied star-formation rates of thousands of solar masses per year. They represent the most intense starbursts in the Universe, yet many are completely optically obscured. Their easy detection at submm wavelengths is due to dust heated by ultraviolet radiation of newly forming stars. When summed up, all of the dusty, star-forming galaxies in the Universe produce an infrared radiation field that has an equal energy density as the direct starlight emission from all galaxies visible at ultraviolet and optical wavelengths. The bulk of this infrared extragalactic background light emanates from galaxies as diverse as gas-rich disks to mergers of intense starbursting galaxies. Major advances in far-infrared instrumentation in recent years, both spacebased and ground-based, has led to the detection of nearly a million DSFGs, yet our understanding of the underlying astrophysics that govern the start and end of the dusty starburst phase is still in nascent stage. This review is aimed at summarizing the current status of DSFG studies, focusing especially on the detailed characterization of the bestunderstood subset (submillimeter galaxies, who were summarized in the last review of this field over a decade ago, Blain et al. 2002), but also the selection and characterization of more recently discovered DSFG populations. We review DSFG population statistics, their physical properties including dust, gas and stellar contents, their environments, and current theoretical models related to the formation and evolution of these galaxies.

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“…An intimate connection between AGN and star formation in galaxies is further suggested by the similar decline in AGN activity (Hasinger et al 2005;Aird et al 2010) and star formation (Hopkins & Beacom 2006) from when the Universe was half its current age to today. Additionally, this connection between galaxy and AGN E-mail: minh.huynh@uwa.edu.au evolution is reflected in the general shift of these processes from high mass galaxies in the distant Universe to low mass galaxies locally (Cowie et al 1996;Hasinger et al 2005;Juneau et al 2005;Mobasher et al 2009), commonly referred to as downsizing. Radio emission can be produced by both AGN and star-forming processes, hence radio wavelengths provide a unique dust-unbiased view of galaxy and AGN evolution.…”

Section: Introductionmentioning

confidence: 99%

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

Huynh¹,

Bell²,

Hopkins³

et al. 2015

Mon. Not. R. Astron. Soc.

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We present a new image of the 5.5 GHz radio emission from the extended Chandra Deep Field South. Deep radio observations at 5.5 GHz were obtained in 2010 and presented in the first data release. A further 76 hours of integration has since been obtained, nearly doubling the integration time. This paper presents a new analysis of all the data. The new image reaches 8.6 µJy rms, an improvement of about 40% in sensitivity. We present a new catalogue of 5.5 GHz sources, identifying 212 source components, roughly 50% more than were detected in the first data release. Source counts derived from this sample are consistent with those reported in the literature for S 5.5GHz > 0.1 mJy but significantly lower than published values in the lowest flux density bins (S 5.5GHz < 0.1 mJy), where we have more detected sources and improved statistical reliability. The 5.5 GHz radio sources were matched to 1.4 GHz sources in the literature and we find a mean spectral index of −0.35 ± 0.10 for S 5.5GHz > 0.5 mJy, consistent with the flattening of the spectral index observed in 5 GHz sub-mJy samples. The median spectral index of the whole sample is α med = −0.58, indicating that these observations may be starting to probe the star forming population. However, even at the faintest levels (0.05 < S 5.5GHz < 0.1 mJy), 39% of the 5.5 GHz sources have flat or inverted radio spectra. Four flux density measurements from our data, across the full 4.5 to 6.5 GHz bandwidth, are combined with those from literature and we find 10% of sources (S 5.5GHz 0.1 mJy) show significant curvature in their radio spectral energy distribution spanning 1.4 to 9 GHz.

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New Insight on Galaxy Formation and Evolution From Keck Spectroscopy of the Hawaii Deep Fields

Cited by 1,623 publications

References 32 publications

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

The DEEP Groth Strip Survey. X. Number Density and Luminosity Function of Field E/S0 Galaxies atz< 1

Dusty star-forming galaxies at high redshift

The ATLAS 5.5 GHz survey of the extendedChandraDeep Field South: the second data release

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