Tracing Ram-Pressure Stripping With Warm Molecular Hydrogen Emission

Sivanandam, Suresh; Rieke, M. J.; Rieke, G. H.

doi:10.1088/0004-637x/796/2/89

Cited by 30 publications

(25 citation statements)

References 77 publications

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“…Enhanced X-ray emission outside NGC 2276, and the bowshock feature on the western edge of NGC 2276's disk was attributed to ram pressure (Rasmussen et al 2006) as similar features have been observed in galaxies with ongoing ram pressure (Iglesias-Paramo & Vilchez 1997;Sivanandam et al 2014;Troncoso Iribarren et al 2016). The high ram pressure acting on NGC 2276 is linked to the unusually high density of the group's inter-galactic medium .…”

Section: Introductionmentioning

confidence: 69%

Two Orders of Magnitude Variation in the Star Formation Efficiency across the Premerger Galaxy NGC 2276

Tomičić

Hughes

Kreckel

et al. 2018

ApJL

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We present the first spatially resolved (∼ 0.5 kpc) measurements of the molecular gas depletion time τ depl across the disk of the interacting spiral galaxy NGC 2276, a system with an asymmetric morphology in various SFR tracers. To estimate τ depl , we use new NOEMA observations of the 12 CO(1-0) emission tracing the bulk molecular gas reservoir in NGC 2276, and extinction-corrected Hα measurements obtained with the PMAS/PPaK integral field unit for robust estimates of the SFR. We find a systematic decrease in τ depl of 1-1.5 dex across the disk of NGC 2276, with a further, abrupt drop in τ depl of ∼1 dex along the galaxy's western edge. The global τ depl in NGC 2776 is τ depl = 0.55 Gyr, consistent with literature measurements for the nearby galaxy population. Such a large range in τ depl on sub-kpc scales has never previously been observed within an individual isolated or pre-merger system. When using a metallicity-dependent molecular gas conversion factor X CO the variation decreases by 0.5 dex. We attribute the variation in τ depl to the influence of galactic-scale tidal forces and ram pressure on NGC 2276's molecular interstellar medium (ISM). Our observations add to the growing body of numerical and observational evidence that galaxy-galaxy interactions significantly modify the molecular gas properties and star-forming activity within galactic disks throughout the interaction, and not just during the final merger phase.

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Section: Introductionmentioning

confidence: 69%

Two Orders of Magnitude Variation in the Star Formation Efficiency across the Premerger Galaxy NGC 2276

Tomičić

Hughes

Kreckel

et al. 2018

ApJL

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“…The dust could be stripped concurrently as spiral galaxies are likely to contain diffuse ionized gas in their halo that is associated with the presence of dust (Howk & Savage 1999;Ménard et al 2010). Moreover, observational evidence for dust stripping in galaxies with likely ongoing ram-pressure stripping has been detected (Crowl et al 2005;Cortese et al 2010a;Sivanandam et al 2014). Therefore, the warmer dust component could be removed with the gas, along with the cool dust associated with the HI (Boselli & Gavazzi 2006;Cortese et al 2010b).…”

Section: A Simple Interpretation For Quenchingmentioning

confidence: 99%

THE PHASE SPACE OF SpARCS CLUSTERS: USING HERSCHEL TO PROBE DUST TEMPERATURE AS A FUNCTION OF ENVIRONMENT AND ACCRETION HISTORY*

Noble

Webb

Yee

et al. 2016

ApJ

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We present a five-band Herschel study (100-500 µm) of three galaxy clusters at z ∼ 1.2 from the Spitzer Adaptation of the Red-Sequence Cluster Survey (SpARCS). With a sample of 120 spectroscopically-confirmed cluster members, we investigate the role of environment on galaxy properties utilizing the projected cluster phase space (line-of-sight velocity versus clustercentric radius), which probes the time-averaged galaxy density to which a galaxy has been exposed. We divide cluster galaxies into phase-space bins of (r/r 200 ) × (∆v/σ v ), tracing a sequence of accretion histories in phase space. Stacking optically star-forming cluster members on the Herschel maps, we measure average infrared star formation rates, and, for the first time in high-redshift galaxy clusters, dust temperatures for dynamically distinct galaxy populations-namely, recent infalls and those that were accreted onto the cluster at an earlier epoch. Proceeding from the infalling to virialized (central) regions of phase space, we find a steady decrease in the specific star formation rate and increase in the stellar age of star-forming cluster galaxies. We perform a probability analysis to investigate all acceptable infrared spectral energy distributions within the full parameter space and measure a ∼ 4σ drop in the average dust temperature of cluster galaxies in an intermediate phase-space bin, compared to an otherwise flat trend with phase space. We suggest one plausible quenching mechanism which may be consistent with these trends, invoking ram-pressure stripping of the warmer dust for galaxies within this intermediate accretion phase.

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“…Increasing AGN feedback from a growing supermassive black hole may shock or eject gas from the galaxy disk, reducing its capacity to form stars (Hopkins et al 2006;Ogle, Lanz, & Appleton 2014). Ram-pressure stripping of the interstellar medium (ISM) by the intercluster medium (ICM) of a galaxy cluster can also remove cold gas (Sivanandam, Rieke, & Rieke 2014).…”

Section: Introductionmentioning

confidence: 99%

Superluminous Spiral Galaxies

Ogle

Lanz

Nader

et al. 2016

ApJ

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We report the discovery of spiral galaxies that are as optically luminous as elliptical brightest cluster galaxies, with r-band monochromatic luminosity L r = 8 − 14L * (4.3 − 7.5 × 10 44 erg s −1 ). These super spiral galaxies are also giant and massive, with diameter D = 57 − 134 kpc and stellar mass M stars = 0.3 − 3.4 × 10 11 M . We find 53 super spirals out of a complete sample of 1616 SDSS galaxies with redshift z < 0.3 and L r > 8L * . The closest example is found at z = 0.089. We use existing photometry to estimate their stellar masses and star formation rates (SFRs). The SDSS and WISE colors are consistent with normal star-forming spirals on the blue sequence. However, the extreme masses and rapid SFRs of 5 − 65M yr −1 place super spirals in a sparsely populated region of parameter space, above the star-forming main sequence of disk galaxies. Super spirals occupy a diverse range of environments, from isolation to cluster centers. We find four super spiral galaxy systems that are late-stage major mergers-a possible clue to their formation. We suggest that super spirals are a remnant population of unquenched, massive disk galaxies. They may eventually become massive lenticular galaxies after they are cut off from their gas supply and their disks fade.

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Tracing Ram-Pressure Stripping With Warm Molecular Hydrogen Emission

Cited by 30 publications

References 77 publications

Two Orders of Magnitude Variation in the Star Formation Efficiency across the Premerger Galaxy NGC 2276

Two Orders of Magnitude Variation in the Star Formation Efficiency across the Premerger Galaxy NGC 2276

THE PHASE SPACE OF SpARCS CLUSTERS: USING HERSCHEL TO PROBE DUST TEMPERATURE AS A FUNCTION OF ENVIRONMENT AND ACCRETION HISTORY*

Superluminous Spiral Galaxies

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