The Nature of Compact Galaxies in the Hubble Deep Field. I. Global Properties

Phillips, Andrew C.; Guzmán, R.; Gallego, J.; Koo, David C.; Lowenthal, James D.; Vogt, Nicole P.; Faber, S. M.; Illingworth, G. D.

doi:10.1086/304796

Cited by 154 publications

(295 citation statements)

References 55 publications

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“…12c are only lower limits). The disky galaxy hd2-264.1 is also compatible with lowluminosity and low-mass spirals, whereas the compact object hd2-264.2 is consistent with the compact narrow emission line galaxy (CNELG) and compact galaxies at higher redshifts of Phillips et al (1997) and Guzmán et al (1997). Interestingly, another compact galaxy from our sample, GSS 084_4515, behaves in a rather different fashion when plotted in these diagrams.…”

Section: No 1 2003mentioning

confidence: 49%

“…12) with those of different galaxy types (both local and at redshifts d1) compiled and published by Phillips et al (1997). The unambiguous spiral-type galaxies of our sample (hd4-656.1, hd4-795.111, GSS 073_1810, and GSS 084_4521) fall in the region spanned by local galaxies of this type in these figures (since these objects are observed face-on, their positions in Fig.…”

Section: No 1 2003mentioning

confidence: 64%

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A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

Cardiel

Elbaz

Schiavon

et al. 2003

ApJ

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We use a sample of seven starburst galaxies at intermediate redshifts (z $ 0:4 and 0.8) with observations ranging from the observed ultraviolet to 1.4 GHz, to compare the star formation rate (SFR) estimators that are used in the different wavelength regimes. We find that extinction-corrected H underestimates the SFR, and the degree of this underestimation increases with the infrared luminosity of the galaxies. Galaxies with very different levels of dust extinction as measured with SFR IR /SFR(H , uncorrected for extinction) present a similar attenuation A[H ], as if the Balmer lines probed a different region of the galaxy than the one responsible for the bulk of the IR luminosity for large SFRs. In addition, SFR estimates derived from [O ii] 3727 match very well those inferred from H after applying the metallicity correction derived from local galaxies. SFRs estimated from the UV luminosities show a dichotomic behavior, similar to that previously reported by other authors in galaxies at zd0:4. Here we extend this result up to z $ 0:8. Finally, one of the studied objects is a luminous compact galaxy (LCG) that may be suffering similar dust-enshrouded star formation episodes. These results highlight the relevance of quantifying the actual L IR of LCGs, as well as that of a much larger and generic sample of luminous infrared galaxies, which will be possible after the launch of SIRTF.

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Section: No 1 2003mentioning

confidence: 49%

Section: No 1 2003mentioning

confidence: 64%

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

Cardiel

Elbaz

Schiavon

et al. 2003

ApJ

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“…The nature of the blue interlopers is intriguing. Preliminary analysis of their spectra shows that most have strong, narrow emission lines, suggesting that they are lowmass starbursts rather than massive star-forming E/S0's (Im et al 2001); they may be similar to the compact narrow emission line galaxies (CNELGs; Koo et al 1994;Guzman et al 1997;Phillips et al 1997).…”

Section: No 1 2002mentioning

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

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142

133

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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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“…Only one such Ðeld exists, and so it is evident that random redshift associations are not the dominant cause of the redshift associations. However, to test whether random redshift associations are signiÐcant, we use published Keck LRIS spectroscopy (Guzman et al 1997 ;Lowenthal et al 1997 ;Phillips et al 1997 ;Vogt et al 1997 ;Cohen et al 2000) out to z \ 1.1 to estimate the likelihood of chance redshift associations. The use of data from the same instrument as used in this study ensures that the data are of comparable quality and have similar systematic problems (sky lines, fringing) over the same redshift range.…”

Section: Spectroscopymentioning

confidence: 99%

Cluster Galaxy Evolution from a New Sample of Galaxy Clusters at 0.3 <z< 0.9

Nelson

Gonzalez

Zaritsky

et al. 2001

ApJ

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We analyze photometry and spectroscopy of a sample of 63 clusters at 0.3 ¹ z ¹ 0.9 drawn from the Las Campanas Distant Cluster Survey to empirically constrain models of cluster galaxy evolution. SpeciÐcally, (1) by combining I-band photometry of 44 of our clusters with that of 19 clusters from the literature, we parameterize the redshift dependence of in the observed frame as We suggest that M I * these observations can be explained with a model in which luminous early-type galaxies (or more precisely, the progenitors of current-day luminous early-type galaxies) form the bulk of their stellar populations at high redshifts and in which many of these galaxies, if not all, accrete mass either in the (Z5) form of evolved stellar populations or gas that causes only a short-term episode of star formation at lower redshifts (1.5 \ z \ 2). Our data are too crude to reach conclusions regarding the evolutionary state of any particular cluster or to investigate whether the morphological evolution of galaxies matches the simple scenario that we discuss, but the statistical nature of this study suggests that the observed evolutionary trends are universal in massive clusters.

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The Nature of Compact Galaxies in the Hubble Deep Field. I. Global Properties

Cited by 154 publications

References 55 publications

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

A Multiwavelength Approach to the Star Formation Rate Estimation in Galaxies at Intermediate Redshifts

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

Cluster Galaxy Evolution from a New Sample of Galaxy Clusters at 0.3 <z< 0.9

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