The structure of elliptical galaxies in the Virgo cluster. Results from the INT Wide Field Survey

Gavazzi, G.; Donati, Alessandro; Cucciati, O.; Sabatini, S.; Boselli, A.; Davies, Jonathan Ivor; Zibetti, S.

doi:10.1051/0004-6361:20034571

Cited by 85 publications

(129 citation statements)

References 42 publications

Supporting

Mentioning

110

Contrasting

Unclassified

Order By: Relevance

“…They are thought to be defunct spiral galaxies that lost their gas through interactions with a more massive companion. We should note that the interpretation we adopt here is not universally accepted in the literature (e.g., Gavazzi et al 2005;Ferrarese et al 2006;Côté et al 2007), but we believe it is well justified by the observations .…”

Section: Bulge Morphologysupporting

confidence: 56%

“…Spheroidal galaxies are typically bluer than elliptical galaxies. For the spheroidal galaxies, we adopt V − I = 1.09 mag, the color of Sbc galaxies listed in Table 3 of Fukugita et al (1995), because spheroidal galaxies are redder than Scd galaxies but bluer than Sa galaxies based on the B − I color (Gavazzi et al 2005;Greene et al 2008). We show the relations between the absolute magnitude of the bulge M I , the effective radius of the bulge r e , and the surface brightness at r e , μ e .…”

Section: The Fundamental Planementioning

confidence: 99%

See 1 more Smart Citation

The Host Galaxies of Low-Mass Black Holes

Jiang

Greene

et al. 2011

ApJ

102

150

View full text Add to dashboard Cite

Using Hubble Space Telescope observations of 147 host galaxies of low-mass black holes (BHs), we systematically study the structures and scaling relations of these active galaxies. Our sample is selected to have central BHs with virial masses of ∼10 5 -10 6 M . The host galaxies have total I-band magnitudes of −23.2 < M I < −18.8 mag and bulge magnitudes of −22.9 < M I < −16.1 mag. Detailed bulge-disk-bar decompositions with GALFIT show that 93% of the galaxies have extended disks, 39% have bars, and 5% have no bulges at all at the limits of our observations. Based on the Sérsic index and bulge-to-total ratio, we conclude that the majority of the galaxies with disks are likely to contain pseudobulges and very few of these low-mass BHs live in classical bulges. The fundamental plane of our sample is offset from classical bulges and ellipticals in a way that is consistent with the scaling relations of pseudobulges. The sample has smaller velocity dispersion at fixed luminosity in the Faber-Jackson plane compared with classical bulges and elliptical galaxies. The galaxies without disks are structurally more similar to spheroidals than to classical bulges according to their positions in the fundamental plane, especially the Faber-Jackson projection. Overall, we suggest that BHs with mass 10 6 M live in galaxies that have evolved secularly over the majority of their history. A classical bulge is not a prerequisite to host a BH.

show abstract

Section: Bulge Morphologysupporting

confidence: 56%

Section: The Fundamental Planementioning

confidence: 99%

The Host Galaxies of Low-Mass Black Holes

Jiang

Greene

et al. 2011

ApJ

102

150

View full text Add to dashboard Cite

show abstract

“…The value of c 2 for giant ellipticals is 1 (Bender et al 1992). For M 86, σ 100 is 2.2 (Smith et al 2000) and R eff is 5.5 kpc (Gavazzi et al 2005) in the B band. CO gas was also found in the V3W and V3WW regions, along an Hα stream that results in the center of M 86, at 9 to 10 kpc away from it (Fig.…”

Section: Notesmentioning

confidence: 98%

Survival of molecular gas in Virgo’s hot intracluster medium: CO near M 86

Dasyra

Combes

Salomé

et al. 2012

A&A

View full text Add to dashboard Cite

We carried out 12 CO(1−0) and 12 CO(2−1) observations of 21 different regions in the vicinity of M 86, NGC 4438, and along the 120 kpc-long, Hα-emitting filamentary trail that connects them, aiming to test whether molecular gas can survive to be transferred from a spiral to an elliptical galaxy in Virgo's 10 7 K intracluster medium (ICM). We targeted Hα-emitting regions that could be associated with the interface between cold molecular clouds and the hot ionized ICM. The data, obtained with the 30 m telescope of the Institut de Radioastronomie Millimétrique, led to the detection of molecular gas close to M 86. CO gas with a recession velocity that is similar to that of the stars, −265 km s −1 , and with a corresponding H 2 mass of 2 × 10 7 M , was detected ∼10 kpc southeast of the nucleus of M 86, near the peak of its H i emission. We argue that it is possible for this molecular gas either to have formed in situ from H i, or to have been stripped from NGC 4438 directly in molecular form. In situ formation is nonetheless negligible for the 7 × 10 6 M of gas detected at 12:26:15.9+12:58:49, at ∼10 kpc northeast of M 86, where no (strong) H i emission is present. This detection provides evidence for the survival of molecular gas in filaments for timescales of ∼100 Myr. An amount equivalent to 5 × 10 7 M of H 2 gas that could be lost to the ICM or to neighboring galaxies was also discovered in the tidal tail northwest of NGC 4438. A scenario in which gas was alternatively brought to M 86 from NGC 4388 was also examined but it was considered unlikely because of the non-detection of CO below or at the H I stream velocities, 2000-2700 km s −1 .

show abstract

“…These galaxies are also older and more α-enhanced than the less luminous counterparts (Kormendy & Illingworth 1982;Nieto et al 1991;Bender et al 1992;Kormendy & Bender 1996;Faber et al 1997;Lauer et al 2005Lauer et al , 2007Emsellem et al 2007;Cappellari et al 2007; Kormendy et al 2009). This dichotomy has been challenged by other authors (Jerjen & Binggeli 1997;Graham & Guzmán 2003;Gavazzi et al 2005). …”

Section: Introductionmentioning

confidence: 98%

Dissecting the morphological and spectroscopic properties of galaxies in the local Universe

Aguerri

Huertas-Company

Alméida

et al. 2012

A&A

View full text Add to dashboard Cite

Aims. We revisit the scaling relations and star-forming histories of local elliptical galaxies using a novel selection method applied to the Sloan Digital Sky Survey DR7. Methods. We combine two probability-based automated spectroscopic and morphological classifications of ∼600 000 galaxies with z < 0.25 to isolate true elliptical galaxies. Our sample selection method does not introduce artificial cuts into the parameters describing the galaxy but instead associates every object with a weight measuring the probability of being in a given spectro-morphological class. Thus, the sample minimizes the selection biases. Results. We show that morphologically defined ellipticals are basically distributed into three spectral classes, which dominate at different stellar masses. The bulk of the population (∼50%) is formed by a well-defined class of galaxies with old stellar populations that formed their stars at very early epochs in a short episode of star formation. They dominate the scaling relations of elliptical galaxies known from previous works and represent the canonical elliptical class. At the low mass end, we find a population of ellipticals with relatively large shapes and smaller velocity dispersions at fixed stellar mass, which seem to have experienced a more recent episode of star formation probably triggered by gas-rich minor mergers. The high mass end tends to be dominated by a third spectral class that is slightly more metal rich and hosts more efficient stellar formation than the reference class. This third class contributes to the curvature in the mass-size relation at high masses reported in previous works. Our method is therefore able to isolate the typical spectra of elliptical galaxies following different evolutionary pathways.

show abstract

The structure of elliptical galaxies in the Virgo cluster. Results from the INT Wide Field Survey

Cited by 85 publications

References 42 publications

The Host Galaxies of Low-Mass Black Holes

The Host Galaxies of Low-Mass Black Holes

Survival of molecular gas in Virgo’s hot intracluster medium: CO near M 86

Dissecting the morphological and spectroscopic properties of galaxies in the local Universe

Contact Info

Product

Resources

About