Optical and Near‐Infrared Color Profiles in Nearby Early‐Type Galaxies and the Implied Age and Metallicity Gradients

Wu, Hong; Shao, Zhengyi; Mo, H. J.; Xia, Xiaoyang; Deng, Z. G.

doi:10.1086/427821

Cited by 109 publications

(177 citation statements)

References 64 publications

(89 reference statements)

Supporting

Mentioning

150

Contrasting

Order By: Relevance

“…In Section 5.3 we have shown that the median colour gradient in our sample is ∼ 2 times steeper than the measured local (U − R) gradient ∇ U−R from Wu et al (2005).…”

Section: Origin and Evolution Of Colour Gradients With Redshiftmentioning

confidence: 54%

“…Tamura & Ohta 2003;Wu et al 2005;Brough et al 2007;Reda et al 2007) as well as in recent simulations (e.g. Hirschmann et al 2015).…”

Section: Methodsmentioning

confidence: 62%

“…The grey arrow in each panel shows the direction of evolution of the median gradient. The red dotted line corresponds to the observed (U − R) gradient at redshift 0 by Wu et al (2005). licity (36 out of 36). We conclude that in the reasonable range of metallicity that we covered, a pure age-driven gradient is not able to match the observed evolution of colour gradient.…”

Section: Case I -Pure Age-driven Gradient Evolutionmentioning

confidence: 98%

“…Wu et al (2005) studied the colour gradients for a sample of 36 local field early-type galaxies from SDSS and 2MASS. Due to a lack of deep U-band imaging, the (U − R) colour gradient is not available in most local galaxy surveys.…”

Section: Colour Gradients In the Passive Cluster Galaxiesmentioning

confidence: 99%

See 3 more Smart Citations

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

View full text Add to dashboard Cite

(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.

show abstract

“…In Section 5.3 we have shown that the median colour gradient in our sample is ∼ 2 times steeper than the measured local (U − R) gradient ∇ U−R from Wu et al (2005).…”

Section: Origin and Evolution Of Colour Gradients With Redshiftmentioning

confidence: 54%

“…Tamura & Ohta 2003;Wu et al 2005;Brough et al 2007;Reda et al 2007) as well as in recent simulations (e.g. Hirschmann et al 2015).…”

Section: Methodsmentioning

confidence: 62%

Section: Case I -Pure Age-driven Gradient Evolutionmentioning

confidence: 98%

Section: Colour Gradients In the Passive Cluster Galaxiesmentioning

confidence: 99%

See 2 more Smart Citations

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

View full text Add to dashboard Cite

show abstract

“…Since the SDSS photometrical survey at uand z-bands are much shallower (Fukugita et al 1996) and i-band used a thinned CCD, an instrumental effect known as the "red halo" in the PSF wings are reported to seriously affected the i-band photometric analysis (e.g., Wu et al 2005). We will only derive gand r-band stellar surface brightness distributions by using the standard task ellipse in…”

Section: Radial Surface Brightness Distributionmentioning

confidence: 99%

Elliptical Galaxies with Emission Lines from the Sloan Digital Sky Survey

Zhao¹,

Gu²,

Peng³

et al. 2006

Chin. J. Astron. Astrophys.

View full text Add to dashboard Cite

We present the results of 11 elliptical galaxies with strong nebular emission lines during our study of star formation history along the Hubble sequence. After removing the dilution from the underlying old stellar populations by use of stellar population synthesis model, we derive the accurate fluxes of all emission lines for these objects, which are later classified with emission line ratios into one Seyfert 2, six LINERs and four HII galaxies. We also identify one HII galaxy (A1216+04) as a hitherto unknown Wolf-Rayet galaxy from the presence of the Wolf-Rayet broad bump at 4650Å. We propose that the star-forming activities in elliptical galaxies are triggered by either galaxy-galaxy interaction or the merging of a small satellite/a massive star cluster, as already suggested by recent numerical simulations.

show abstract

The Color-Magnitude Relations of Late-type Spiral Galaxies and Their Disks

Shao

Shen

et al. 2009

Chinese Astronomy and Astrophysics

View full text Add to dashboard Cite

Optical and Near‐Infrared Color Profiles in Nearby Early‐Type Galaxies and the Implied Age and Metallicity Gradients

Cited by 109 publications

References 64 publications

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

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

Elliptical Galaxies with Emission Lines from the Sloan Digital Sky Survey

The Color-Magnitude Relations of Late-type Spiral Galaxies and Their Disks

Contact Info

Product

Resources

About