Constraints on the Early Formation of Field Elliptical Galaxies

Barger, A. J.; Cowie, L. L.; Trentham, Neil; Fulton, E.; Hu, E. M.; Songaila, A.; Hall, Donald N. B.

doi:10.1086/300675

Cited by 124 publications

(205 citation statements)

References 43 publications

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“…This CDF-N observation has also allowed us to place strong constraints on two potential extended X-ray-emitting systems, ClG 1236+6215 and VLA J123725+621128. Both systems lie at high redshift and, from their undetected status, may still be in the early stages of dynamical evolution, having not yet -Chandra ACIS-I adaptively smoothed soft-band contours of the undetected cluster of galaxies ClG 1236+6215 overlaid on the I-band image of Barger et al (1999). The properties of the image (e.g., contours and bar) are identical to those described in Fig.…”

Section: Basic Nature Of the Extended X-ray Sourcesmentioning

confidence: 80%

“…As a consistency check for the SExtractor photometry, we matched our sources to sources in the catalog of Barger et al (1999); we found good agreement, with 1 deviations of .0.25. As expected, the largest deviations were always near the detection threshold of the images.…”

Section: Optical Images and Photometrymentioning

confidence: 82%

“…Simulations using the I-band image yielded significant (greater than 90% confidence level) overdensities for sources 3, 4, and 5, although the small number Barger et al (1999), with the exceptions of sources 1 and 6, which lie outside the field of view of the I-band image and instead are overlaid on the R-band image of Liu et al (1999). Each contour indicates an increase in X-ray flux by a factor of ffiffi ffi 2 p .…”

Section: Tests Of Clusteringmentioning

confidence: 98%

“…These include the HK 0 -, I-, V-, and B-band images of Barger et al (1999) 12 and the U n -, G-, and R-band images of Steidel & Hamilton (1993), all of which cover an %9 0 Â 9 0 region surrounding the HDF-N, as well as the R-band image of Liu et al (1999), which extends over the entire CDF-N region. The HK 0 -, I-, R-, R-, V-, G-, B-, and U n -band images have %2 detection limits of 21.2, 25.5, 25.6, 23.0, 26.5, 26.4, 26.3, and 25.0, respectively.…”

Section: Optical Images and Photometrymentioning

confidence: 99%

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The Chandra Deep Field North Survey. IX. Extended X-Ray Sources

Bauer¹,

Alexander²,

Brandt³

et al. 2002

The Astronomical Journal

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The %1 Ms Chandra Deep Field North observation is used to study the extended X-ray sources in the region surrounding the Hubble Deep Field North (HDF-N), yielding the most sensitive probe of extended X-ray emission at cosmological distances to date. A total of six such sources are detected, the majority of which align with small numbers of optically bright galaxies. Their angular sizes, band ratios, and X-ray luminosities-assuming they lie at the same distances as the galaxies coincident with the X-ray emission-are generally consistent with the properties found for nearby groups of galaxies. One source is notably different and is likely to be a poor-to-moderate X-ray cluster at high redshift (i.e., z & 0.7). This source has a large angular extent, a double-peaked X-ray morphology, and an overdensity of unusual objects [very red objects, optically faint (I ! 24) radio and X-ray sources]. Another of the six sources is coincident with several z % 1.01 galaxies located within the HDF-N itself, including the FR I radio galaxy VLA J123644+621133, and is likely to be a group or poor cluster of galaxies at that redshift. We are also able to place strong constraints on the optically detected cluster of galaxies ClG 1236+6215 at z = 0.85 and the wide-angle-tailed radio galaxy VLA J123725+621128 at z $ 1-2; both sources are expected to have considerable associated diffuse X-ray emission, and yet they have rest-frame 0.5-2.0 keV X-ray luminosities of .3 Â 10 42 and .(3-15) Â 10 42 ergs s À1 , respectively. The environments of both sources are either likely to have a significant deficit of hot intracluster gas compared with local clusters of galaxies, or they are X-ray groups. We find the surface density of extended X-ray sources in this observation to be 167 þ97 À67 deg À2 at a limiting soft-band flux of %3 Â 10 À16 ergs cm À2 s À1 . No evolution in the X-ray luminosity function of clusters is needed to explain this value.

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Section: Basic Nature Of the Extended X-ray Sourcesmentioning

confidence: 80%

Section: Optical Images and Photometrymentioning

confidence: 82%

Section: Tests Of Clusteringmentioning

confidence: 98%

Section: Optical Images and Photometrymentioning

confidence: 99%

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The Chandra Deep Field North Survey. IX. Extended X-Ray Sources

Bauer¹,

Alexander²,

Brandt³

et al. 2002

The Astronomical Journal

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“…Zepf 1998, Barger et al 1999, based on the very low surface density of EROs recovered in K-selected samples. However, others found results consistent with a constant comoving density, even up to z ∼ 2 (e.g.…”

mentioning

confidence: 99%

Is the Deficit of Z > 1 Field Ellipticals Real?

Daddi

2001

The Evolution of Galaxies

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Abstract. The results of a 700 arcmin 2 survey for EROs are presented. The sky distribution of EROs is very inhomogeneous and their two point correlation function shows a very high amplitude, a factor of 10 larger than that of the field galaxy population. Such a clustering can explain the strong variance found in previous works, and provides evidence that ERO are mostly made of high-z ellipticals. The surface density of EROs found in our large survey is in good agreement with that expected for passively evolving ellipticals formed at high redshift (z > ∼ 2.5).

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Deep Near-Infrared Imaging Surveys and the Stellar Content of High Redshift Galaxies

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Deep, near-infrared imaging surveys have been motivated by the desire to study the rest-frame optical properties and stellar content of galaxies at high redshift. Here we briefly review their history, and illustrate one application, using HST NICMOS imaging of the Hubble Deep Field North to examine the rest-frame optical luminosities and colors of galaxies at 2 < z < 3, and to constrain their stellar masses. The rest-frame B-band luminosity density at z ≈ 2.5 is similar to that in the local universe, but the galaxies are evidently less massive, with rapid star formation and low mass-to-light ratios. There are few candidates for red, nonstar-forming galaxies at these redshifts to the HDF/NICMOS limits. We estimate a stellar mass density at 2 < z < 3 that is ∼ 5% of the present-day value, with an upper bound of ≤ 30%. Future headway will come from wide-field ground-based surveys, multiplexing infrared spectrographs, and new space-based facilities such as HST/WFC3 and SIRTF/IRAC.

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Constraints on the Early Formation of Field Elliptical Galaxies

Cited by 124 publications

References 43 publications

The Chandra Deep Field North Survey. IX. Extended X-Ray Sources

The Chandra Deep Field North Survey. IX. Extended X-Ray Sources

Is the Deficit of Z > 1 Field Ellipticals Real?

Deep Near-Infrared Imaging Surveys and the Stellar Content of High Redshift Galaxies

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