RED NUGGETS AT<i>z</i>∼ 1.5: COMPACT PASSIVE GALAXIES AND THE FORMATION OF THE KORMENDY RELATION

Damjanov, Ivana; McCarthy, Patrick J.; Abraham, Roberto; Glazebrook, Karl; Yan, Haojing; Mentuch, Erin; Borgne, D. Le; Savaglio, S.; Crampton, D.; Murowinski, Richard; Juneau, Stéphanie; Carlberg, R. G.; Jørgensen, Inger; Roth, Kathy; Chen, Hsiao‐Wen; Marzke, Ronald O.

doi:10.1088/0004-637x/695/1/101

Cited by 316 publications

(362 citation statements)

References 71 publications

Supporting

Mentioning

341

Contrasting

Unclassified

Order By: Relevance

“…5 and following). We used the recent intermediate redshift sample , the classic high redshift sample of Damjanov et al (2009), the new high redshift sample of Belli et al (2014), and the catalogue of van de , which contains a composition of various high redshift samples, such as Bezanson et al (2013), van Dokkum et al (2009), Onodera et al (2012, Cappellari et al (2009), Newman et al (2010, van der Wel et al (2008), Blakeslee et al (2006), Toft et al (2012), and their own work. We cannot perform a comparison with these datasets in every figure, because sometimes some samples do not contain the required parameters.…”

Section: Resultsmentioning

confidence: 99%

“…Based on the previous observation of quiescent high-redshift galaxies (Kriek et al 2006, van Dokkum et al (2008) found that there are already fully formed early-type galaxies with scale radii that are much smaller and stellar masses that are much higher than any object known in the local universe. For comparison, we used several samples of these galaxies at high redshifts, such as those of Damjanov et al (2009, and Belli et al (2014), and also at intermediate redshifts as in Zahid et al (2015). Many of these galaxies must have evolved, most likely by mergers, into more regular early-type galaxies.…”

Section: Discussionmentioning

confidence: 99%

“…The high redshift sample of Belli et al (2014) is indicated by red Xs. Open brown nabla symbols mark the high redshift galaxies of Damjanov et al (2009). Open magenta circles indicate the intermediate redshift sample of Zahid et al (2015).…”

Section: The Mass-to-light Ratiomentioning

confidence: 99%

“…We used a variety of high redshift samples for comparison, such as the classic high redshift sample of Damjanov et al (2009) Toft et al (2012), and their own work. In the size-stellar mass plane (see Fig.…”

Section: Comparison To Intermediate and High Redshift Samplesmentioning

confidence: 99%

See 3 more Smart Citations

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Saulder

Bosch

Mieske

2015

A&A

View full text Add to dashboard Cite

Context. Passive galaxies at high redshift are much smaller than equally massive early types today. If this size evolution is caused by stochastic merging processes, then a small fraction of the compact galaxies should persist until today. Up to now it has not been possible to systematically identify the existence of such objects in Sloan Digital Sky Survey (SDSS). Aims. We aim at finding potential survivors of these compact galaxies in SDSS, as targets for more detailed follow-up observations. Methods. From the virial theorem, it is expected that for a given mass, compact galaxies have stellar velocity dispersion higher than the mean owing to their smaller sizes. Therefore velocity dispersion, coupled with size (or mass), is an appropriate method of selecting relics, independent of the stellar population properties. Based on these considerations, we designed a set of criteria the use the distribution of early-type galaxies from SDSS on the log 10 (R 0 )−log 10 (σ 0 ) plane to find the most extreme objects on it. We thus selected compact massive galaxy candidates by restricting them to high velocity dispersions σ 0 > 323.2 km s −1 and small sizes R 0 < 2.18 kpc. Results. We find 76 galaxies at 0.05 < z < 0.2, which have properties that are similar to the typical quiescent galaxies at high redshift. We discuss how these galaxies relate to average present-day early-type galaxies. We study how well these galaxies fit on well-known local universe relations of early-type galaxies, such as the fundamental plane, the red sequence, or mass-size relations. As expected from the selection criteria, the candidates are located in an extreme corner of the mass-size plane. However, they do not extend as deeply into the so-called zone of exclusion as some of the red nuggets found at high redshift, since they are a factor 2−3 less massive on a given intrinsic scale size. Several of our candidates are close to the size resolution limit of SDSS, but are not so small that they are classified as point sources. We find that our candidates are systematically offset on a scaling relation compared to the average early-type galaxies, but still within the general range of other early-type galaxies. Furthermore, our candidates are similar to the mass-size range expected for passive evolution of the red nuggets from their high redshift to the present. Conclusions. The 76 selected candidates form an appropriate set of objects for further follow-up observations. They do not constitute a separate population of peculiar galaxies, but form the extreme tail of a continuous distribution of early-type galaxies. We argue that selecting a high-velocity dispersion is the best way to find analogues of compact high redshift galaxies in the local universe.

show abstract

Section: Resultsmentioning

confidence: 99%

Section: Discussionmentioning

confidence: 99%

Section: The Mass-to-light Ratiomentioning

confidence: 99%

Section: Comparison To Intermediate and High Redshift Samplesmentioning

confidence: 99%

See 2 more Smart Citations

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Saulder

Bosch

Mieske

2015

A&A

View full text Add to dashboard Cite

show abstract

“…This leads to an inside-out quenching process into a compact, passive "red nugget", the likely progenitor of the centre of an early-type galaxy today. The observational basis for this picture is becoming solid, both for the red-nugget phenomenon (Trujillo et al 2006a,b;van Dokkum et al 2008;Damjanov et al 2009Damjanov et al , 2011Newman et al 2010;Bruce et al 2012;Whitaker et al 2012;van Dokkum et al 2014) and for their potential bluenugget progenitors (Barro et al 2013(Barro et al , 2014aBruce et al 2014;Nelson et al 2014;Williams et al 2014;Tacchella et al 2015a). The theory, partly based on the same simulations that we analyse here, is also becoming robust (Dekel & Burkert 2014;Tacchella et al 2015b,c;Zolotov et al 2015).…”

Section: Introductionmentioning

confidence: 99%

Evolution of galaxy shapes from prolate to oblate through compaction events

Tomassetti

Dekel²,

Mandelker³

et al. 2016

Mon. Not. R. Astron. Soc.

View full text Add to dashboard Cite

We study the evolution of global shapes of galaxies using cosmological simulations. The shapes refer to the components of dark matter (DM), stars and gas at the stellar half-mass radius. Most galaxies undergo a characteristic compaction event into a blue nugget at z ∼ 2 − 4, which marks the transition from a DM-dominated central body to a self-gravitating baryonic core. We find that in the high-z, DM-dominated phase, the stellar and DM systems tend to be triaxial, preferentially prolate and mutually aligned. The elongation is supported by an anisotropic velocity dispersion that originates from the assembly of the galaxy along a dominant large-scale filament. We estimate that torques by the dominant halo are capable of inducing the elongation of the stellar system and its alignment with the halo. Then, in association with the transition to self-gravity, small-pericenter orbits puff up and the DM and stellar systems evolve into a more spherical and oblate configuration, aligned with the gas disc and associated with rotation. This transition typically occurs when the stellar mass is ∼ 10 9 M and the escape velocity in the core is ∼ 100 km s −1 , indicating that supernova feedback may be effective in keeping the core DM-dominated and the system prolate. The early elongated phase itself may be responsible for the compaction event, and the transition to the oblate phase may be associated with the subsequent quenching in the core.

show abstract

Chemodynamical Simulations of Galaxies

Kobayashi

2010

Galaxies and Their Masks

View full text Add to dashboard Cite

Abstract. We simulate the formation and evolution of galaxies with a self-consistent 3D hydrodynamical model including star formation, supernova feedback, and chemical enrichment. Hypernova feedback plays an essential role not only in solving the [Zn/Fe] problem, but also reproducing the cosmic star formation rate history and the mass-metallicity relations. In a MilkyWay type galaxy, kinematics and chemical abundances are different in bulge, disk, and thick disk because of different star formation histories and the contribution of Type Ia Supernovae.

show abstract

RED NUGGETS ATz∼ 1.5: COMPACT PASSIVE GALAXIES AND THE FORMATION OF THE KORMENDY RELATION

Cited by 316 publications

References 71 publications

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Dozens of compact and high velocity-dispersion, early-type galaxies in Sloan Digital Sky Survey

Evolution of galaxy shapes from prolate to oblate through compaction events

Chemodynamical Simulations of Galaxies

Contact Info

Product

Resources

About