SHOCK-ENHANCED C+EMISSION AND THE DETECTION OF H2O FROM THE STEPHAN'S QUINTET GROUP-WIDE SHOCK USINGHERSCHEL

Appleton, P. N.; Guillard, P.; Boulanger, F.; Cluver, Michelle; Ogle, Patrick; Falgarone, É.; Forêts, G. Pineau des; O’Sullivan, Ewan; Duc, Pierre–Alain; Gallagher, S. C.; Gao, Yu; Jarrett, T. H.; Konstantopoulos, I. S.; Lisenfeld, U.; Lord, S. D.; Lu, N.; Peterson, Bradley W.; Struck, Curtis; Sturm, E.; Tuffs, R.; Valchanov, I.; Werf, P. van der; Xu, Kevin

doi:10.1088/0004-637x/777/1/66

Cited by 99 publications

(84 citation statements)

References 81 publications

(178 reference statements)

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“…However, for low turbulent velocities, it becomes difficult to distinguish between this mechanism and low-density PDRs. The extreme L [CII] /LFIR ratios Appleton et al (2013) find for the intergalactic filament in Stephan's Quintet are ∼ 30× higher than those observed in the SPT sample. Smaller shockionised regions may still contribute significantly to the observed [CII] emission.…”

Section: Other Contributions To the [Cii] Emissioncontrasting

confidence: 57%

“…Malhotra et al 1997, Luhman et al 1998, Maiolino et al 2009Stacey et al 2010;Graciá-Carpio et al 2011;Sargsyan et al 2012). Various physical explanations for this trend have been proposed, including an increased ionisation parameter (Malhotra et al 2001;Abel et al 2009;Graciá-Carpio et al 2011), collisional de-excitation of [CII] (Appleton et al 2013) and non-PDR contributions to the FIR luminosity (Luhman et al 2003), possibly from AGN (Sargsyan et al 2012). Stacey et al (2010) argued that the lower [CII]/FIR ratio can be explained by the fact that the star-formation in local ULIRGs is confined and vigorous (leading to high G0), while in the most distant objects, the star-formation is very large-scale, but of lower intensity (i.e.…”

Section: The [Cii]/fir Luminosity Deficitmentioning

confidence: 99%

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The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

154

224

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We present [CII] observations of 20 strongly lensed dusty star forming galaxies at 2.1 < z < 5.7 using APEX and Herschel. The sources were selected on their 1.4 mm flux (S 1.4 mm > 20 mJy) from the South Pole Telescope survey, with far-infrared (FIR) luminosities determined from extensive photometric data. The [CII] line is robustly detected in 17 sources, all but one being spectrally resolved. Eleven out of 20 sources observed in [CII] also have low-J CO detections from ATCA. A comparison with midand high-J CO lines from ALMA reveals consistent [CII] and CO velocity profiles, suggesting that there is little differential lensing between these species. The [CII], low-J CO and FIR data allow us to constrain the properties of the interstellar medium. We find [CII] to CO(1-0) luminosity ratios in the SPT sample of 5200 ± 1800, with significantly less scatter than in other samples. This line ratio can be best described by a medium of [CII] and CO emitting gas with a higher [CII] than CO excitation temperature, high CO optical depth τ CO (1-0) 1, and low to moderate [CII] optical depth τ [CII] 1. The geometric structure of photodissociation regions allows for such conditions.

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Section: Other Contributions To the [Cii] Emissioncontrasting

confidence: 57%

Section: The [Cii]/fir Luminosity Deficitmentioning

confidence: 99%

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

Gullberg

Breuck

Vieira

et al. 2015

Monthly Notices of the Royal Astronomical Society

154

224

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“…Given the small offset of the line peaks from the systemic [CI]2-1 redshift, only 100 to 200 km s −1 , and the average line width of 290 km s −1 of the two H 2 O lines, it is likely that the width of the lines represents the dispersion of the clouds and that mechanical energy is being dissipated within the dense molecular gas. Not only H 2 O, but also the detection of strong mid-infrared H 2 emission (Ogle et al 2012), suggest excitation of molecules in lowvelocity shocks (see discussion in Guillard et al 2009;Appleton et al 2013). Moreover, we emphasise that, owing to the position of the H 2 O emission in our bandpass, higher negative offset velocity emission, such as that from companion #10, would not lie within our bandpass (Kuiper et al 2011).…”

Section: Cooling Of the Post-shock Gas Owing To Slow Shocks In Molecumentioning

confidence: 76%

ALMA finds dew drops in the dusty spider’s web

Gullberg

Lehnert

Breuck

et al. 2016

A&A

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We present 0 . 5 resolution ALMA detections of the observed 246 GHz continuum, [CI] 3 P 2 → 3 P 1 fine structure line ([CI]2-1), CO(7-6), and H 2 O lines in the z = 2.161 radio galaxy MRC1138-262, the so-called Spiderweb galaxy. We detect strong [CI]2-1 emission both at the position of the radio core, and in a second component ∼4 kpc away from it. The 1100 km s −1 broad [CI]2-1 line in this latter component, combined with its H 2 mass of 1.6 × 10 10 M , implies that this emission must come from a compact region <60 pc, possibly containing a second active galactic nucleus (AGN). The combined H 2 mass derived for both objects, using the [CI]2-1 emission, is 3.3 × 10 10 M . The total CO(7-6)/[CI]2-1 line flux ratio of 0.2 suggests a low excitation molecular gas reservoir and/or enhanced atomic carbon in cosmic ray dominated regions. We detect spatially-resolved H 2 O 2 11 −2 02 emission -for the first time in a high-z unlensed galaxy -near the outer radio lobe to the east, and near the bend of the radio jet to the west of the radio galaxy. No underlying 246 GHz continuum emission is seen at either position. We suggest that the H 2 O emission is excited in the cooling region behind slow (10-40 km s −1 ) shocks in dense molecular gas (10 3−5 cm −3 ). The extended water emission is likely evidence of the radio jet's impact on cooling and forming molecules in the post-shocked gas in the halo and inter-cluster gas, similar to what is seen in low-z clusters and other high-z radio galaxies. These observations imply that the passage of the radio jet in the interstellar and inter-cluster medium not only heats gas to high temperatures, as is commonly assumed or found in simulations, but also induces cooling and dissipation, which can lead to substantial amounts of cold dense molecular gas. The formation of molecules and strong dissipation in the halo gas of MRC1138-262 may explain both the extended diffuse molecular gas and the young stars observed around MRC1138-262.

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“…HCG92 (Stephan's Quintet) is one example where a galaxy has collided with previously tidally stripped HI plume, creating a powerful molecularrich shock. In that system almost all the gas is stripped from the galaxies and lies in the IGM (see Guillard et al 2012;Appleton et al 2013).…”

Section: The Dust Masses Of the Hcg Late-type Galaxiesmentioning

confidence: 99%

“…The best studied example is Stephan's Quintet (SQ = HCG92), where HI and molecular studies show that almost all of the cold interstellar medium (ISM) now resides in the intragroup medium (Williams et al 2002;Gao & Xu 2000;Guillard et al 2012). Strong dissipative processes, in addition to gravity, are clearly at work on a large scale in this system, leading to extensive shock heating in the interfaces between galaxies and the intragroup medium, as is evident by the presence of hot X-ray gas, warm molecular hydrogen, and diffuse ionized carbon (Trinchieri et al 2005;O'Sullivan et al 2009;Appleton et al 2006;Cluver et al 2010;Appleton et al 2013).…”

Section: Introductionmentioning

confidence: 98%

Herschelobservations of Hickson compact groups of galaxies: Unveiling the properties of cold dust

Bitsakis

Charmandaris

Appleton

et al. 2014

A&A

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We present a Herschel far-infrared and sub-millimetre (sub-mm) study of a sample of 120 galaxies in 28 Hickson compact groups (HCGs). Fitting their UV to sub-mm spectral energy distributions with the model of da Cunha et al. (2008), we accurately estimate the dust masses, luminosities, and temperatures of the individual galaxies. We find that nearly half of the late-type galaxies in dynamically "old" groups, those with more than 25% of early-type members and redder UV-optical colours, also have significantly lower dustto-stellar mass ratios compared to those of actively star-forming galaxies of the same mass found both in HCGs and in the field. Examining their dust-to-gas mass ratios, we conclude that dust was stripped out of these systems as a result of the gravitational and hydrodynamic interactions, experienced owing to previous encounters with other group members. About 40% of the early-type galaxies (mostly lenticulars), in dynamically "old" groups, display dust properties similar to those of the UV-optical red late-type galaxies. Given their stellar masses, star formation rates, and UV-optical colours, we suggest that red late-type and dusty lenticular galaxies represent transition populations between blue star-forming disk galaxies and quiescent early-type ellipticals. On the other hand, both the complete absence of any correlation between the dust and stellar masses of the dusty ellipticals and their enhanced star formation activity, suggest the increase in their gas and dust content due to accretion and merging. Our deep Herschel observations also allow us to detect the presence of diffuse cold intragroup dust in 4 HCGs. We also find that the fraction of 250 μm emission that is located outside of the main bodies of both the red late-type galaxies and the dusty lenticulars is 15−20% of their integrated emission at this band. All these findings are consistent with an evolutionary scenario in which gas dissipation, shocks, and turbulence, in addition to tidal interactions, shape the evolution of galaxies in compact groups.

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SHOCK-ENHANCED C⁺EMISSION AND THE DETECTION OF H₂O FROM THE STEPHAN'S QUINTET GROUP-WIDE SHOCK USINGHERSCHEL

Cited by 99 publications

References 81 publications

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

The nature of the [C ii] emission in dusty star-forming galaxies from the SPT survey

ALMA finds dew drops in the dusty spider’s web

Herschelobservations of Hickson compact groups of galaxies: Unveiling the properties of cold dust

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