A Dozen New Galaxies Caught in the Act: Gas Stripping and Extended Emission Line Regions in the Coma Cluster

Yagi, Masafumi; Yoshida, Michitoshi; Komiyama, Yutaka; Kashikawa, Nobunari; Furusawa, Hisanori; Okamura, S.; Graham, Alister W.; Miller, Neal A.; Carter, David; Mobasher, Bahram; Jogee, Shardha

doi:10.1088/0004-6256/140/6/1814

Cited by 170 publications

(252 citation statements)

References 62 publications

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“…Examples of Hα tails can be found in the Virgo cluster (NGC 4522, Kenney & Koopmann 1999) and in Abell 1367 (97-079 and 97-073, Gavazzi et al 2001; the BIG group, Cortese et al 2006). A recent survey of the Coma cluster by Yagi et al (2010) shows that almost all blue galaxies in the core of this cluster reveal tails and distorted Hα profiles when observed with a 10-m class telescope.…”

Section: Resultsmentioning

confidence: 99%

“…For instance within the Yagi et al (2010) sample, only two objects show signs of star formation along the trail (GMP3016 and RB199). VCC 1217 so far represents the closest and smallest known object with this unusual feature.…”

Section: Resultsmentioning

confidence: 99%

“…Long narrow Hα tails, stretching up to 150 Kpc, are reported in the Virgo cluster (Kenney & Koopmann 1999), Abell 1367 (Gavazzi et al 2001;Cortese et al 2006), and Coma cluster (Yagi et al 2010) associated to infalling galaxies. There is, however, little evidence that star formation ignites in the stripped wakes, except in a few cases.…”

Section: Introductionmentioning

confidence: 95%

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Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

Fumagalli

Gavazzi

Scaramella

et al. 2011

A&A

123

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Context. A complex of Hα emitting blobs with strong FUV excess is associated to the dIrr galaxy VCC 1217/IC 3418 (Hester et al. 2010, ApJ, 716, L14), and extends up to 17 Kpc in the southeast direction. These outstanding features can be morphologically divided into diffuse filaments and compact knots, where most of the star formation activity traced by Hα takes place. Aims. We investigate the properties of the galaxy and the blobs using a multiwavelength approach to constrain their origin. Methods. We collected publicly available data in UV and Hα and observed the scene in the optical U, g, r, i bands with LBT. The photometric data allows evaluation of the star formation rate and performance of a SED fitting separately for the galaxy and the blobs in order to constrain their stellar population age. Moreover we analyzed the color and luminosity profile of the galaxy and its spectrum to investigate its recent interaction with the Virgo cluster. Results. Our analysis confirms that the most plausible mechanism for the formation of the blobs is ram pressure stripping by the Virgo cluster IGM. The galaxy colors, luminosity profile and SED are consistent with a sudden gas depletion in the last few hundred Myr. The SED fitting of the blobs constrains their ages in <400 Myr.

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Section: Resultsmentioning

confidence: 99%

Section: Resultsmentioning

confidence: 99%

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Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

Fumagalli

Gavazzi

Scaramella

et al. 2011

A&A

123

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“…Multiphase hydrodynamical simulations indicate that gas ablation in all its phases (from diffuse atomic to dense molecular gas) can take place at all galactic radii if ram pressure stripping is sufficiently strong, as indeed is the case in rich clusters of galaxies such as Virgo (Tonnesen & Bryan 2009). There is also observational evidence indicating that ram pressure stripping is efficient up to the cluster virial radius (Scott et al 2012;Gavazzi et al 2001;Yagi et al 2010;Fossati et al 2012). It is thus reasonable to assume that ram pressure stripping can completely remove the gas of the ISM on timescales of 1.5 Gyr in galaxies within the virial radius 5 .…”

Section: Implications On the Star Formation History Of Cluster Galaxiesmentioning

confidence: 99%

Cold gas properties of theHerschelReference Survey

Boselli

Cortese

Boquien

et al. 2014

A&A

176

250

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The Herschel Reference Survey is a complete volume-limited, K-band-selected sample of nearby objects including Virgo cluster and isolated objects. Using a recent compilation of Hi and CO data for this sample we study the effects of the cluster environment on the molecular gas content of spiral galaxies. With the subsample of unperturbed field galaxies, we first identify the stellar mass as the scaling variable that traces the total molecular gas mass of galaxies better. We show that, on average, Hi-deficient galaxies are significantly offset (4σ) from the M(H 2 ) vs. M star relation for Hi-normal galaxies. We use the M(H 2 ) vs. M star scaling relation to define the H 2 -deficiency parameter as the difference, on logarithmic scale, between the expected and observed molecular gas mass for a galaxy of given stellar mass. The H 2 -deficiency parameter shows a weak and scattered relation with the Hi-deficiency parameter, here taken as a proxy for galaxy interactions with the surrounding cluster environment. We also show that, as for the atomic gas, the extent of the molecular disc decreases with increasing Hi-deficiency. All together, these results show that cluster galaxies have, on average, a lower molecular gas content than similar objects in the field. Our analysis indicates that ram pressure stripping is the physical process responsible for this molecular gas deficiency. The slope of the H 2 − de f vs. Hi − de f relation is less than unity, while the D(Hi)/D(i) vs. Hi − de f relation is steeper than the D(CO)/D(i) vs. Hi − de f relation, thereby indicating that the molecular gas is removed less efficiently than the atomic gas. This result can be understood if the atomic gas is distributed on a relatively flat disc that is more extended than the stellar disc. It is thus less anchored to the gravitational potential well of the galaxy than the molecular gas phase, which is distributed on an exponential disc with a scalelength r CO 0.2r 24.5 (g). There is a clear trend between the NUV-i colour index, which is a proxy for the specific star formation activity, and the H 2 -deficiency parameter, which suggests that molecular gas removal quenches the activity of star formation. This causes galaxies migrate from the blue cloud to the green valley and, eventually, to the red sequence. The total gas-consumption timescale of gas deficient cluster galaxies is comparable to that of isolated, unperturbed systems. The total gas depletion timescale determined by considering the recycled fraction is τ gas,R 3.0−3.3 Gyr, which is significantly larger than the typical timescale for total gas removal in a ram pressure stripping process, indicated by recent hydrodynamical simulations to be τ RP 1.5 Gyr. The comparison of these timescales suggests that ram pressure, rather than a simple stop of the infall of pristine gas from the halo, will be the dominant process driving the future evolution of these cluster galaxies.

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“…Another typical feature of a ram-pressure stripped tail is the absence of a stellar counterpart. Moreover, galaxies that are infalling in rich clusters occasionally show stripped gas with associated star formation (Cortese et al 2007), as evident from their ultraviolet (UV) (Smith et al 2011), Hα (Yagi et al 2010), and X-ray emission (Sun et al 2010). A remarkable example is the dwarf irregular (dIrr) galaxy VCC 1217, which shows an extended tail of bright knots and of diffuse emission in the UV light (Hester et al 2010;Fumagalli et al 2011), which is associated to star formation triggered by the interaction with the intergalactic medium.…”

Section: Introductionmentioning

confidence: 99%

Stripped gas as fuel for newly formed H ii regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS

Battaia

Gavazzi

Fumagalli

et al. 2012

A&A

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Context. We study the peculiar interacting galaxy system of VCC 1249/M 49 located in the core of the Virgo B subcluster. Owing to a recent interaction between the dwarf galaxy VCC 1249 and the halo gas of the elliptical galaxy M 49, neutral hydrogen has been displaced from the interstellar medium of this dwarf into the Virgo intracluster medium. Observations also reveal multiple compact star-forming regions (aka H ii regions) that are embedded in this H i cloud, with a projected separation up to 13 kpc from VCC 1249 in the northwest direction. Aims. Motivated by recent near-ultraviolet imaging from the GALEX Ultraviolet Virgo Cluster Survey (GUViCS) of the VCC 1249/M 49 system that shows significant ongoing/recent star formation in the compact regions, we aim to constrain the origin of these outlying H ii regions with a multi-wavelength approach. Methods. Using deep optical (u, g, i, z) imaging from the Next Generation Virgo Cluster Survey (NGVS) and new Hα imaging obtained at the San Pedro Martir observatory together with Keck long-slit spectroscopy, we characterize the star formation rates, ages, and metallicity of VCC 1249 and its outlying compact regions. Moreover, we analyze the color and luminosity profile of the galaxy to investigate its recent interaction with M 49. Results. Our new observations indicate that VCC 1249 underwent a recent interaction with M 49 in which both ram-pressure stripping and tidal interaction occured. The joint action of the two mechanisms led to the removal of the H i gas from the interstellar medium of VCC 1249, while the gravitational tides triggered the stellar tail and counter-tail of VCC 1249. Our stellar population synthesis analysis reveals that the star formation in this galaxy was truncated around 200 Myr ago and that the outlying H ii regions were born in situ ≈10 Myr ago out of pre-enriched gas removed from the dwarf galaxy. These observations also reveal that interactions between central and satellite galaxies similar to those between VCC 1249/M 49 may be an effective way of dispersing metals into the halos of massive galaxies.

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A Dozen New Galaxies Caught in the Act: Gas Stripping and Extended Emission Line Regions in the Coma Cluster

Cited by 170 publications

References 62 publications

Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

Constraining the ages of the fireballs in the wake of the dIrr galaxy VCC 1217/IC 3418

Cold gas properties of theHerschelReference Survey

Stripped gas as fuel for newly formed H ii regions in the encounter between VCC 1249 and M 49: a unified picture from NGVS and GUViCS

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