Ionised gas structure of 100 kpc in an over-dense region  of the galaxy group COSMOS-Gr30 at z ~ 0.7

Épinat, B.; Contini, T.; Finley, Hayley; Boogaard, Leindert; Guérou, Adrien; Brinchmann, Jarle; Carton, David; Michel-Dansac, Léo; Bacon, Roland; Cantalupo, Sebastiano; Carollo, M.; Hamer, Stephen; Kollatschny, W.; Krajnović, Davor; Marino, R. A.; Richard, Johan; Soucail, G.; Weilbacher, Peter M.; Wisotzki, L.

doi:10.1051/0004-6361/201731877

Cited by 48 publications

(50 citation statements)

References 120 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…However, in addition to individual galaxies associated with DLA, the MUSE data also uncovered spatially extended line-emitting gas, detected in Hα, Hβ, [O III], and [O II], across the galaxy group. The emitting morphology is consistent with the gas being stripped from members of the galaxy group, similar to what was found in other group environments (e.g., Epinat et al 2018;Johnson et al 2018). One of the denser streams passes directly in front of the QSO with kinematics consistent with the absorption profiles revealed in the QSO echelle spectrum.…”

Section: Absorption Spectra Of the Qsosupporting

confidence: 88%

A Giant Intragroup Nebula Hosting a Damped Absorber at z = 0.313

Chen

Boettcher

Johnson

et al. 2019

ApJL

View full text Add to dashboard Cite

This paper reports the discovery of spatially-extended line-emitting nebula, reaching to ≈ 100 physical kpc (pkpc) from a damped Lyα absorber (DLA) at z DLA = 0.313 along the sightline toward QSO PKS 1127−145 (z QSO = 1.188). This DLA was known to be associated with a galaxy group of dynamical mass M group ∼ 3 × 10 12 M , but its physical origin remained ambiguous. New wide-field integral field observations revealed a giant nebula detected in [O II], Hβ, [O III], Hα, and [N II] emission, with the line-emitting gas following closely the motions of group galaxies. One of the denser streams passes directly in front of the QSO with kinematics consistent with the absorption profiles recorded in the QSO echelle spectra. The emission morphology, kinematics, and line ratios of the nebula suggest that shocks and turbulent mixing layers, produced as a result of stripped gaseous streams moving at supersonic speed across the ambient hot medium, contribute significantly to the ionization of the gas. While the DLA may not be associated with any specific detected member of the group, both the kinematic and dust properties are consistent with the DLA originating in streams of gas stripped from sub-L * group members at 25 pkpc from the QSO sightline. This study demonstrates that gas stripping in low-mass galaxy groups is effective in releasing metal-enriched gas from star-forming regions, producing absorption systems in QSO spectra, and that combining absorption and emission-line observations provides an exciting new opportunity for studying gas and galaxy co-evolution. of all baryons in the universe (e.g., Miralda-Escudé et al. 1996;Fukugita 2004), serving as a reservoir of materials for sustaining the growth of galaxies while maintaining a record of feedback from previous episodes of star formation and active galactic nuclei (AGN) activity. A comprehensive understanding of the origin and

show abstract

Section: Absorption Spectra Of the Qsosupporting

confidence: 88%

A Giant Intragroup Nebula Hosting a Damped Absorber at z = 0.313

Chen

Boettcher

Johnson

et al. 2019

ApJL

View full text Add to dashboard Cite

show abstract

“…Signatures of cool gas coming from this type of interactions have been observed directly in emission in different massive halos (e.g. Epinat et al 2018;Johnson et al 2018). The cool gas stripped by the satellite could eventually fall down towards the central massive galaxy, in a journey compatible with the motion described by our model.…”

Section: Alternative Originsmentioning

confidence: 95%

Cool circumgalactic gas of passive galaxies from cosmological inflow

Afruni

Fraternali

Pezzulli

2019

A&A

View full text Add to dashboard Cite

The circumgalactic medium (CGM) of galaxies consists of a multiphase gas with components at very different temperatures, from 10 4 K to 10 7 K. One of the greatest puzzle about this medium is the presence of a large amount of low-temperature (T ∼ 10 4 K) gas around quiescent early-type galaxies (ETGs). Using semi-analytical parametric models, we describe the cool CGM around massive, low-redshift ETGs as the cosmological accretion of gas into their dark matter halos, resulting in an inflow of clouds from the external parts of the halos to the central galaxies. We compare our predictions with the observations of the COS-LRG collaboration. We find that inflow models can successfully reproduce the observed kinematics, the number of absorbers and the column densities of the cool gas. Our MCMC fit returns masses of the cool clouds of about 10 5 M and shows that they must evaporate during their journey due to hydrodynamic interactions with the hot gas. We conclude that the cool gas present in the halos of ETGs likely cannot reach the central regions and feed the galaxy star formation, thus explaining why these passive objects are no longer forming stars.

show abstract

“…We determined galaxy parameters, such as stellar mass, star formation rate (SFR), and extinction, from spectral energy distribution models using the FAST code (Kriek et al 2009) as described in Epinat et al (2018) for a similar dataset in the COS-MOS field with deep imaging data from the UV to the near-IR. Stellar masses and SFR are calculated assuming a Chabrier (2003) IMF.…”

Section: Other Datamentioning

confidence: 99%

Evidence for ram-pressure stripping in a cluster of galaxies at z = 0.7

Boselli

Épinat

Contini

et al. 2019

A&A

Self Cite

View full text Add to dashboard Cite

MUSE observations of the cluster of galaxies CGr32 (M 200 2 × 10 14 M ) at z = 0.73 reveal the presence of two massive star forming galaxies with extended tails of diffuse gas detected in the [O ii]λλ3727-3729Å emission-line doublet. The tails, which have a cometary shape with a typical surface brightness of a few 10 −18 erg s −1 cm −2 arcsec −2 , extend up to 100 kpc (projected distance) from the galaxy discs and are not associated to any stellar component. All this observational evidence suggests that the gas has been removed during a ram-pressure stripping event. This observation is thus the first evidence that dynamical interactions with the intracluster medium were active when the Universe had only half of its present age. The density of the gas derived using the observed [O ii]λ3729/[O ii]λ3726 line ratio implies a very short recombination time, suggesting that a source of ionisation is necessary to keep the gas ionised within the tail.

show abstract

Ionised gas structure of 100 kpc in an over-dense region of the galaxy group COSMOS-Gr30 at z ~ 0.7

Cited by 48 publications

References 120 publications

A Giant Intragroup Nebula Hosting a Damped Absorber at z = 0.313

A Giant Intragroup Nebula Hosting a Damped Absorber at z = 0.313

Cool circumgalactic gas of passive galaxies from cosmological inflow

Evidence for ram-pressure stripping in a cluster of galaxies at z = 0.7

Contact Info

Product

Resources

About