UV‐Optical Colors as Probes of Early‐Type Galaxy Evolution

Kaviraj, Sugata; Schawinski, Kevin; Devriendt, Julien; Ferreras, Ignacio; Khochfar, Sadegh; Yoon, Suk-Jin; Yi, Sukyoung K.; Deharveng, J. M.; Boselli, A.; Barlow, Tom A.; Conrow, T.; Forster, Karl; Friedman, Peter G.; Martin, D. Christopher; Morrissey, Patrick; Neff, Susan G.; Schiminovich, David; Seibert, Mark; Small, Todd; Wyder, Ted K.; Bianchi, Luciana; Donas, J.; Heckman, Timothy M.; Lee, Y.-W.; Madore, Barry F.; Milliard, B.; Rich, R. Michael; Szalay, Alexander S.

doi:10.1086/516633

Cited by 324 publications

(412 citation statements)

References 82 publications

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“…It is conceivable that type i+ ETGs have previously been forming stars at a much higher pace − a conjecture in qualitative agreement with the presence of ionized gas disks in intermediate-redshift ETGs (Jaffé et al 2014) − and are now seen in an advanced stage of a prolonged, gradually declining SF process (e.g., Kaviraj et al 2007). The Gyr-long inside-out growth of ETGs is also suggested by the outwardly increasing luminosity contribution of stellar populations younger than 5 Gyr (G15b) and their by ∼0.1−0.25 dex lower light-weighted age in their periphery (e.g., González Delgado et al 2015), following a general trend for Hubble-type galaxies (e.g., Pérez et al 2013).…”

Section: Spiral-like Sf Features In the Etg Peripherymentioning

confidence: 65%

Spiral-like star-forming patterns in CALIFA early-type galaxies

Gomes

Papaderos

Vı́lchez

et al. 2015

A&A

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Based on a combined analysis of SDSS imaging and CALIFA integral field spectroscopy data, we report on the detection of faint (24 < µ r mag/ < 26) star-forming spiral-arm-like features in the periphery of three nearby early-type galaxies (ETGs). These features are of considerable interest because they document the still ongoing inside-out growth of some local ETGs and may add valuable observational insight into the origin and evolution of spiral structure in triaxial stellar systems. A characteristic property of the nebular component in the studied ETGs, classified i+, is a two-radial-zone structure, with the inner zone that displays faint (EW(Hα) 1 Å) low-ionization nuclear emission-line region (LINER) properties, and the outer one (3 Å < EW(Hα) < ∼ 20 Å) H-region characteristics. This spatial segregation of nebular emission in two physically distinct concentric zones calls for an examination of aperture effects in studies of type i+ ETGs with single-fiber spectroscopic data.

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Section: Spiral-like Sf Features In the Etg Peripherymentioning

confidence: 65%

Spiral-like star-forming patterns in CALIFA early-type galaxies

Gomes

Papaderos

Vı́lchez

et al. 2015

A&A

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“…There are indications that intermediatemass early-type galaxies have a low level of ongoing star formation (e.g. Kaviraj et al 2007;Schawinski et al 2007;Salim & Rich 2010), but it seems unlikely that it is sufficiently strong to affect our conclusions.…”

Section: Discussionmentioning

confidence: 84%

Evolution of the luminosity-to-halo mass relation of LRGs from a combined analysis of SDSS-DR10+RCS2

Uitert¹,

Cacciato

Hoekstra

et al. 2015

A&A

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We study the evolution of the luminosity-to-halo mass relation of luminous red galaxies (LRGs). We selected a sample of 52 000 LOWZ and CMASS LRGs from the Baryon Oscillation Spectroscopic Survey (BOSS) SDSS-DR10 in the ∼450 deg 2 that overlaps with imaging data from the second Red-sequence Cluster Survey (RCS2), grouped them into bins of absolute magnitude and redshift and measured their weak-lensing signals. The source redshift distribution has a median of 0.7, which allowed us to study the lensing signal as a function of lens redshift. We interpreted the lensing signal using a halo model, from which we obtained the halo masses as well as the normalisations of the mass-concentration relations. The concentration of haloes that host LRGs is consistent with dark-matter-only simulations once we allow for miscentering or satellites in the modelling. The slope of the luminosity-to-halo mass relation has a typical value of 1.4 and does not change with redshift, but we find evidence for a change in amplitude: the average halo mass of LOWZ galaxies increases by 25 +16 −14 % between z = 0.36 and 0.22 to an average value of (6.43 ± 0.52) × 10 13 h −1 70 M . If we extend the redshift range using the CMASS galaxies and assume that they are the progenitors of the LOWZ sample, the average mass of LRGs increases by 80 +39 −28 % between z = 0.6 and 0.2.

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“…The latter galaxies might have an increased contribution to the emission at the PACS wavelengths from circumstellar dust or from stochastic heating, or a more intense interstellar radiation field, associated with postmain-sequence phases of the evolution of super-solar metallicity low-intermediate-mass stars or, alternatively, recent star formation activity (e.g. Kaviraj et al 2007). The higher dust temperature in more massive galaxies could also be due to conductive heat transfer from the X-ray gas (Sparks et al 2012, and references therein).…”

Section: Dust Vs Starsmentioning

confidence: 99%

TheHerschelVirgo Cluster Survey

Alighieri

Bianchi

Pappalardo

et al. 2013

A&A

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Aims. We study the dust content of a large optical input sample of 910 early-type galaxies (ETG) in the Virgo cluster, also extending to the dwarf ETG, and examine the results in relation to those on the other cold ISM components. Methods. We have searched for far-infrared emission in all galaxies in the input sample using the 250 μm image of the Herschel Virgo Cluster Survey (HeViCS). This image covers a large fraction of the cluster with an area of ∼55 square degrees. For the detected ETG we measured fluxes in five bands from 100 to 500 μm, and estimated the dust mass and temperature with modified black-body fits. Results. Dust is detected above the completeness limit of 25.4 mJy at 250 μm in 46 ETG, 43 of which are in the optically complete part of the input sample. In addition, dust is present at fainter levels in another six ETG. We detect dust in the four ETG with synchrotron emission, including M 87. Dust appears to be much more concentrated than stars and more luminous ETG have higher dust temperatures. Considering only the optically complete input sample and correcting for the contamination by background galaxies, dust detection rates down to the 25.4 mJy limit are 17% for ellipticals, about 40% for lenticulars (S0 + S0a), and around 3% for dwarf ETG. Dust mass does not correlate clearly with stellar mass and is often much greater than expected for a passive galaxy in a closedbox model. The dust-to-stars mass ratio anticorrelates with galaxy luminosity, and for some dwarf ETG reaches values as high as for dusty late-type galaxies. In the Virgo cluster slow rotators appear more likely to contain dust than fast ones. Comparing the dust results with those on Hi there are only eight ETG detected both in dust and in Hi in the HeViCS area; 39 have dust but only an upper limit on Hi, and eight have Hi but only an upper limit on dust. The locations of these galaxies in the cluster are different, with the dusty ETG concentrated in the densest regions, while the Hi rich ETG are at the periphery.

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UV‐Optical Colors as Probes of Early‐Type Galaxy Evolution

Cited by 324 publications

References 82 publications

Spiral-like star-forming patterns in CALIFA early-type galaxies

Spiral-like star-forming patterns in CALIFA early-type galaxies

Evolution of the luminosity-to-halo mass relation of LRGs from a combined analysis of SDSS-DR10+RCS2

TheHerschelVirgo Cluster Survey

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