The evolution of disk galaxies and the origin of S0 galaxies

Larson, Richard B.; Tinsley, Beatrice M.; Caldwell, Christy

doi:10.1086/157917

Cited by 1,546 publications

(1,559 citation statements)

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“…The main physical processes acting on the gas component are starvation (Larson, Tinsley, & Caldwell 1980) and ram pressure (Gunn & Gott 1972), while the change in mass and/or morphology are mostly ascribed to harassment (Moore et al 1996) and strong tidal interactions (Aguerri & González-García 2009). What the dominant processes in clusters are is still an open question, and the analysis of the faint end of the LF helps to put some constrains.…”

Section: Environmental Influence On Dwarfsmentioning

confidence: 99%

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

Agulli¹,

Aguerri²,

Sánchéz-Janssen³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present a new deep spectroscopic catalogue for Abell 85, within 3.0 × 2.6 Mpc 2 and down to M r ∼ M * r +6. Using the Visible Multi-Object Spectrograph at the Very Large Telescope and the AutoFiber 2 at the William Herschel Telescope, we obtained almost 1430 new redshifts for galaxies with m r ≤ 21 mag and µ e,r ≤ 24 mag arcsec −2 . These redshifts, together with SDSS-DR6 and NED spectroscopic information, result in 460 confirmed cluster members. This data set allows the study of the luminosity function (LF) of the cluster galaxies covering three orders of magnitudes in luminosities. The total and radial LFs are best modelled by a double Schechter function. The normalized LFs show that their bright (M r ≤ −21.5) and faint (M r ≥ −18.0) ends are independent of clustercentric distance and similar to the field LFs unlike the intermediate luminosity range (−21.5 ≤ M r ≤ −18.0). Similar results are found for the LFs of the dominant types of galaxies: red, passive, virialized and early-infall members. On the contrary, the LFs of blue, star-forming, non-virialized and recent-infall galaxies are well described by a single Schechter function. These populations contribute to a small fraction of the galaxy density in the innermost cluster region. However, in the outskirts of the cluster, they have similar densities to red, passive, virialized and early-infall members at the LF faint end. These results confirm a clear dependence of the colour and star formation of Abell 85 members in the cluster centric distance.

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Section: Environmental Influence On Dwarfsmentioning

confidence: 99%

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

Agulli¹,

Aguerri²,

Sánchéz-Janssen³

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Recent IFU observations demonstrate that many nearby spiral galaxies show negative gradients in stellar ages and metallicities, supporting this inside-out picture (González Delgado et al 2014;Sánchez-Blázquez et al 2014;Li et al 2015;Belfiore et al 2017;Goddard et al 2017). On the other hand, if "nurture" dominates galaxy evolution, external processes such as ram-pressure stripping (Gunn & Gott 1972), high speed galaxy encounters (Moore et al 1996), galaxy mergers (Mihos & Hernquist 1994), and "strangulation" (Larson et al 1980;Balogh et al 2000;Peng et al 2015) are responsible for quenching. In this picture, star formation quenching is likely to occur globally or in the outer regions of galaxies first due to the lack of continuous supply for the cold gas reservoir.…”

Section: Introductionmentioning

confidence: 99%

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

Lin

Belfiore

Pan

et al. 2017

ApJ

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We study the role of cold gas in quenching star formation in the green valley by analyzing ALMA 12 CO (1-0) observations of three galaxies with resolved optical spectroscopy from the MaNGA survey. We present resolution-matched maps of the star formation rate and molecular gas mass. These data are used to calculate the star formation efficiency (SFE) and gas fraction ( f gas ) for these galaxies separately in the central "bulge" regions and outer disks. We find that, for the two galaxies whose global specific star formation rate (sSFR) deviates most from the star formation main sequence, the gas fraction in the bulges is significantly lower than that in their disks, supporting an "inside-out" model of galaxy quenching. For the two galaxies where SFE can be reliably determined in the central regions, the bulges and disks share similar SFEs. This suggests that a decline in f gas is the main driver of lowered sSFR in bulges compared to disks in green valley galaxies. Within the disks, there exist common correlations between the sSFR and SFE and between sSFR and f gas on kiloparsec scales-the local SFE or f gas in the disks declines with local sSFR. Our results support a picture in which the sSFR in bulges is primarily controlled by f gas , whereas both SFE and f gas play a role in lowering the sSFR in disks. A larger sample is required to confirm if the trend established in this work is representative of the green valley as a whole.

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“…Couch et al 1994), which evolve into spheroidal systems observed in local clusters. Larson et al (1980) proposed the process of galaxy strangulation as another means of transforming field spirals into cluster ellipticals and S0s. Gas from infalling galaxies escapes its host because of tidal forces created by the cluster potential well.…”

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confidence: 99%

The rise and fall of star formation in z ∼ 0.2 merging galaxy clusters

Stroe¹,

Sobral²,

Dawson³

et al. 2015

Monthly Notices of the Royal Astronomical Society

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CIZA J2242.8+5301 ('Sausage') and 1RXS J0603.3+4213 ('Toothbrush') are two lowredshift (z ∼ 0.2), massive (∼ 2 × 10 15 M ), post-core passage merging clusters, which host shock waves traced by diffuse radio emission. To study their star-formation properties, we uniformly survey the 'Sausage' and 'Toothbrush' clusters in broad and narrow band filters and select a sample of 201 and 463 line emitters, down to a rest-frame equivalent width (13Å). We robustly separate between Hα and higher redshift emitters using a combination of optical multi-band (B, g, V, r, i, z) and spectroscopic data. We build Hα luminosity functions for the entire cluster region, near the shock fronts, and away from the shock fronts and find striking differences between the two clusters. In the dynamically younger, 1 Gyr old 'Sausage' cluster we find numerous (59) Hα emitters above a star-formation rate (SFR) of 0.17 M yr −1 surprisingly located in close proximity to the shock fronts, embedded in very hot intra-cluster medium plasma. The SFR density for the cluster population is at least at the level of typical galaxies at z ∼ 2. Down to the same star-formation rate, the possibly dynamically more evolved 'Toothbrush' cluster has only 9 Hα galaxies. The cluster Hα galaxies fall on the SFRstellar mass relation z ∼ 0.2 for the field. However, the 'Sausage' cluster has an Hα emitter density > 20 times that of blank fields. If the shock passes through gas-rich cluster galaxies, the compressed gas could collapse into dense clouds and excite star-formation for a few 100 Myr. This process ultimately leads to a rapid consumption of the molecular gas, accelerating the transformation of gas-rich field spirals into cluster S0s or ellipticals.

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The evolution of disk galaxies and the origin of S0 galaxies

Cited by 1,546 publications

References 0 publications

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

Deep spectroscopy of nearby galaxy clusters – I. Spectroscopic luminosity function of Abell 85

SDSS-IV MaNGA-resolved Star Formation and Molecular Gas Properties of Green Valley Galaxies: A First Look with ALMA and MaNGA

The rise and fall of star formation in z ∼ 0.2 merging galaxy clusters

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