Radially extended kinematics and stellar populations of the massive ellipticals NGC 1600, NGC 4125, and NGC 7619

SB, Pu; Saglia, R. P.; Fabricius, M.; Thomas, Jens; Bender, Ralf; Han, Zhanwen

doi:10.1051/0004-6361/201014395

Cited by 39 publications

(50 citation statements)

References 95 publications

(169 reference statements)

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“…To do this we observed 5 stars from the Lick/IDS library using the same instrumental configuration used for the science objects and derived the offsets between our data and the Lick/IDS system. The comparison of our data with the Lick standard systems can be found in Pu et al (2010 , Fig. 4).…”

Section: R (Arcsec)mentioning

confidence: 85%

Stellar kinematics and populations out to 1.5 effective radii in the elliptical galaxy NGC 4636

Han

2011

Res. Astron. Astrophys.

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We present high quality long slit spectra along the major and minor axes out to 1.5 effective radius (R e ) of the massive galaxy NGC4636 taken by Hobby-Eberly Telescope (HET). Using Fourier Correlation Quotient (FCQ) method, we measured the stellar line-of-sight velocity distribution along the axes. Furthermore, six Lick/IDS indices (Hβ, Mgb, Fe 5015 , Fe 5270 , Fe 5335 , Fe 5406 ) are derived from the clean spectrum. By comparing the measured absorption line strengths with the predictions of Simple Stellar Populations (SSP) models, we derived ages, total metallicity and α abundance profiles of the galaxy. This galaxy presents old and [α/Fe] over abundant stellar populations. Indeed, using the SSP model, we obtained the broadband color profiles. The theoretical colors match well with the measured colors and present red sharp peaks at the galaxy center. The sharp peaks of the colors are mainly shaped by the high metallicity in the galaxy center. Interestingly, the galaxy has steep negative metallicity gradients, but trend flattens outwards. This result likly suggests that the center and outer regions of the galaxy formed through different formation process.

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Section: R (Arcsec)mentioning

confidence: 85%

Stellar kinematics and populations out to 1.5 effective radii in the elliptical galaxy NGC 4636

Han

2011

Res. Astron. Astrophys.

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“…In a similar way elliptical galaxy (e.g., Carollo et al 1995;Mehlert et al 2000;Pu et al 2010) and cluster of galaxy velocity dispersion profiles (e.g., Lokas et al 2006), exibits a remarkable flattenings at large radii where a Keplerian falloff would be expected. These deviations, ascribed Based on observations collected at the European Southern Observatory, Chile .…”

Section: Introductionmentioning

confidence: 86%

Testing Newtonian gravity with distant globular clusters: NGC 1851 and NGC 1904

Scarpa

Marconi

Carraro

et al. 2010

A&A

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Context. Globular clusters are useful for testing the validity of Newtonian dynamics in the low acceleration regime typical of galaxies, without the complications of non-baryonic dark matter. In the absence of disturbing effects, such as tidal heating, the velocity dispersion of globular clusters is expected to vanish at large radii. If this is not observed, and in particular if, as observed in elliptical galaxies, the dispersion is found to be constant at large radii below a certain threshold acceleration, this might indicate a breakdown of Newtonian dynamics. Aims. To minimize the effects of tidal heating that can increase the velocity dispersion at large radii, we study the velocity dispersion profile of two distant globular clusters, NGC 1851 and NGC 1904. Methods. The velocity dispersion profile is derived from accurate radial velocity measurements, obtained at the ESO 8m VLT telescope with the FLAMES multi-object spectrograph. Reliable data for 184 and 146 bona fide cluster star members were obtained for NGC 1851 and NGC 1904, respectively. Results. These data allow us to trace the velocity dispersion profile to ∼2r 0 , where r 0 is the radius at which the cluster internal acceleration of gravity is a 0 ∼ 10 −8 cm s −2 . It is found that in both clusters the velocity dispersion is maximal at the center, decreases moving outward, and then becomes constant beyond ∼r 0 . Since the distance of these clusters from the Milky Way is large, the observed flattening of the velocity dispersion profile cannot be ascribed to tidal heating effects, as proposed in the case of nearer globular clusters. Conclusions. These results are in full agreement with those found for another five globular clusters previously investigated as part of this project. Taken together, our results for these 7 clusters support the claim that the velocity dispersion is constant beyond r 0 , irrespectively of the specific physical properties of the clusters: mass, size, dynamical history, and distance from the Milky Way. The strong similarity to the constant velocity dispersion observed in elliptical galaxies beyond r 0 is indicative of a common origin for this phenomenon in the two class of objects, and possibly a breakdown of Newtonian dynamics below a 0 .

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“…In order to take into account the average age difference between field and cluster passive galaxies (e.g. Thomas et al 2005Thomas et al , 2010, we evolve the gradients of Wu et al (2005) for an additional 2 Gyr with Bruzual & Charlot (2003) SSP models (assuming an age gradient of −0.05 and a metallicity gradient of −0.2 consistent with the literature (La Barbera et al 2005;Wu et al 2005)). The extrapolated value (∇ U−R = −0.20) is very close to the one for local ETGs.…”

Section: Colour Gradients In the Passive Cluster Galaxiesmentioning

confidence: 99%

“…NGC 4889 in Coma cluster Coccato, Gerhard & Arnaboldi 2010) as well as in field ellipticals (e.g. Pu et al 2010). More recent studies have extended the age and metallicity measurements to large radii (∼ 8 − 10R e , for example in La ) and revealed that the outer age or metallicity gradients at 1 − 2R e are distinct from those in the inner region (e.g.…”

Section: Implications and Limitationsmentioning

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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Radially extended kinematics and stellar populations of the massive ellipticals NGC 1600, NGC 4125, and NGC 7619

Cited by 39 publications

References 95 publications

Stellar kinematics and populations out to 1.5 effective radii in the elliptical galaxy NGC 4636

Stellar kinematics and populations out to 1.5 effective radii in the elliptical galaxy NGC 4636

Testing Newtonian gravity with distant globular clusters: NGC 1851 and NGC 1904

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

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