WFPC2 Observations of the Hubble Deep Field South

Casertano, Stefano; Mello, Duília de; Dickinson, Mark; Ferguson, Henry C.; Fruchter, A. S.; González-Lópezlira, Rosa A.; Heyer, I.; Hook, R. N.; Levay, Zolt; Lucas, Ray A.; Mack, J.; Makidon, Russell B.; Mutchler, Max; Smith, T. E.; Stiavelli, M.; Wiggs, Michael S.; Williams, Robert E.

doi:10.1086/316851

Cited by 285 publications

(318 citation statements)

References 33 publications

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“…HST point-spread function is wavelength dependent, in order to properly compare observed and modeled gradients, we convolved each modeled surface brightness profile with a onedimensional radial Gaussian point-spread function of different FWHM in the and bands (Casertano et al 2000).…”

Section: Resultsmentioning

confidence: 99%

The Origin of Blue Cores in Hubble Deep Field E/S0 Galaxies

Menanteau

Jiménez

Matteuccí

2001

The Astrophysical Journal

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In this Letter we address the problem of the origin of blue cores and inverse color gradients in early-type galaxies reported in the Hubble Deep Field-North and Hubble Deep Field-South by Menanteau, Abraham, & Ellis. We use a multizone single-collapse model. This model accounts for the observed blue cores by adopting a broad spread in formation redshifts for elliptical galaxies, allowing some of these galaxies to begin forming no more than ∼1 Gyr before the redshift of observation. The single-zone collapse model then produces cores that are bluer than the outer regions because of the increase of the local potential well toward the center, which makes star formation more extended in the central region of the galaxy. We compare the predicted V 606 ϪI 814 (r) color gradients with those observed using the redshift of formation ( ) of the elliptical as the only free parameter.z F We find that the model can account with relatively good agreement for the blue cores and inverse color gradients found in many spheroidals and at the same time for the red and smooth color profiles reported. Based on the model, our analysis suggests two populations of field elliptical galaxies, one formed recently, within Շ1 Gyr, and another much older, formed տ4 Gyr since the redshift of observation.

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Section: Resultsmentioning

confidence: 99%

The Origin of Blue Cores in Hubble Deep Field E/S0 Galaxies

Menanteau

Jiménez

Matteuccí

2001

The Astrophysical Journal

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“…The star-galaxy classification is performed using a standard MAG AUTO-MU MAX plane selection (see L07 & J12 for more details). Finally, to overcome the pattern-dependent correlations introduced by the drizzling process between neighbouring pixels, which artificially reduce the noise level of co-added drizzled images, we apply the remedy used by L07: simply scaling up the noise level in each pixel by the same constant F A ≈ 0.316, defined by Casertano et al (2000).…”

Section: Weak-lensing Constraintsmentioning

confidence: 99%

Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies

Richard¹,

Jauzac²,

Limousin³

et al. 2014

Monthly Notices of the Royal Astronomical Society

219

271

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Citation for published item:i h rdD tF nd t uz D wF nd vimousinD wF nd tulloD iF nd gl¡ ementD fF nd i elingD rF nd unei D tFE F nd etekD rF nd x t r j nD F nd ig miD iF nd vivermoreD F nd fowerD F @PHIRA 9w ss nd m gni( tion m ps for the ru le p e eles ope prontier pields lusters X impli tions for highEredshift studiesF9D wonthly noti es of the oy l estronomi l o ietyFD RRR @IAF ppF PTVEPVWF Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTExtending over three Hubble Space Telescope (HST) cycles, the Hubble Frontier Fields (HFF) initiative constitutes the largest commitment ever of HST time to the exploration of the distant Universe via gravitational lensing by massive galaxy clusters. Here, we present models of the mass distribution in the six HFF cluster lenses, derived from a joint strong-and weak-lensing analysis anchored by a total of 88 multiple-image systems identified in existing HST data. The resulting maps of the projected mass distribution and of the gravitational magnification effectively calibrate the HFF clusters as gravitational telescopes. Allowing the computation of search areas in the source plane, these maps are provided to the community to facilitate the exploitation of forthcoming HFF data for quantitative studies of the gravitationally lensed population of background galaxies. Our models of the gravitational magnification afforded by the HFF clusters allow us to quantify the lensing-induced boost in sensitivity over blank-field observations and predict that galaxies at z > 10 and as faint as m(AB) = 32 will be detectable, up to 2 mag fainter than the limit of the Hubble Ultra Deep Field.

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“…Due to the nature of the drizzle process, the resulting drizzled images have correlated pixelto-pixel noise. To correct for this we follow Casertano et al (2000) to apply a scaling factor to the weight maps. Absolute WCS calibrations of the drizzled images are derived using GAIA (Graphical Astronomy and Image analysis Tool) in the Starlink library (Berry et al 2013) with Guide Star Catalog II (GSC-II) (Lasker et al 2008).…”

Section: Hst Imagingmentioning

confidence: 99%

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

Chan

Beifiori

Mendel

et al. 2016

Mon. Not. R. Astron. Soc.

137

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(2016) 'Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 at z = 1.39.', Monthly notices of the Royal Astronomical Society., 458 (3). pp. 3181-3209. Further information on publisher's website: Additional information: Use policyThe full-text may be used and/or reproduced, and given to third parties in any format or medium, without prior permission or charge, for personal research or study, educational, or not-for-pro t purposes provided that:• a full bibliographic reference is made to the original source • a link is made to the metadata record in DRO • the full-text is not changed in any way The full-text must not be sold in any format or medium without the formal permission of the copyright holders.Please consult the full DRO policy for further details. ABSTRACTWe analyse the sizes, colour gradients, and resolved stellar mass distributions for 36 massive and passive galaxies in the cluster XMMUJ2235-2557 at z = 1.39 using optical and nearinfrared Hubble Space Telescope imaging. We derive light-weighted Sérsic fits in five HST bands (i 775 , z 850 ,Y 105 , J 125 , H 160 ), and find that the size decreases by ∼ 20% going from i 775 to H 160 band, consistent with recent studies. We then generate spatially resolved stellar mass maps using an empirical relationship between M * /L H 160 and (z 850 − H 160 ) and use these to derive mass-weighted Sérsic fits: the mass-weighted sizes are ∼ 41% smaller than their restframe r-band counterparts compared with an average of ∼ 12% at z ∼ 0. We attribute this evolution to the evolution in the M * /L H 160 and colour gradient. Indeed, as expected, the ratio of mass-weighted to light-weighted size is correlated with the M * /L gradient, but is also mildly correlated with the mass surface density and mass-weighted size. The colour gradients (∇ z−H ) are mostly negative, with a median value of ∼ 0.45 mag dex −1 , twice the local value. The evolution is caused by an evolution in age gradients along the semi-major axis (a), with ∇ age = d log(age)/d log(a) ∼ −0.33, while the survival of weaker colour gradients in old, local galaxies implies that metallicity gradients are also required, with ∇ Z = d log(Z)/d log(a) ∼ −0.2. This is consistent with recent observational evidence for the inside-out growth of passive galaxies at high redshift, and favours a gradual mass growth mechanism, such as minor mergers.

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WFPC2 Observations of the Hubble Deep Field South

Cited by 285 publications

References 33 publications

The Origin of Blue Cores in Hubble Deep Field E/S0 Galaxies

The Origin of Blue Cores in Hubble Deep Field E/S0 Galaxies

Mass and magnification maps for the Hubble Space Telescope Frontier Fields clusters: implications for high-redshift studies

Sizes, colour gradients and resolved stellar mass distributions for the massive cluster galaxies in XMMUJ2235-2557 atz= 1.39

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