H i content in galaxies in loose groups

Sengupta, Chandreyee; Balasubramanyam, R.

doi:10.1111/j.1365-2966.2006.10307.x

Cited by 51 publications

(57 citation statements)

References 37 publications

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“…15. An indication that some (presumably enriched) gas has been removed from our group galaxies by other means than SN outflows is provided by the factor of 2–3 deficiency in H i mass derived for the spirals in NGC 5044 and NGC 7619 compared to field spirals of similar optical morphology and size (Sengupta & Balasubramanyam 2006). In addition, evidence for ongoing or past stripping associated with galaxy–ICM interactions is present in a few of our groups (Rasmussen, Ponman & Mulchaey 2006; Mendel et al 2009).…”

Section: Origin and Fate Of Icm Metals In Groupsmentioning

confidence: 95%

Temperature and abundance profiles of hot gas in galaxy groups - II. Implications for feedback and ICM enrichment

Rasmussen

Ponman

2009

Monthly Notices of the Royal Astronomical Society

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We investigate the history of galactic feedback and chemical enrichment within a sample of 15 X‐ray bright groups of galaxies, on the basis of the inferred Fe and Si distributions in the hot gas and the associated metal masses produced by core‐collapse and Type Ia supernovae (SNe). Most of these cool‐core groups show a central Fe and Si excess, which can be explained by prolonged enrichment by SN Ia and stellar winds in the central early‐type galaxy alone, but with tentative evidence for additional processes contributing to core enrichment in hotter groups. Inferred metal mass‐to‐light ratios inside r500 show a positive correlation with total group mass but are generally significantly lower than in clusters, due to a combination of lower global intracluster medium (ICM) abundances and gas‐to‐light ratios in groups. This metal deficiency is present for products from both SN Ia and SN II, and suggests that metals were either synthesized, released from galaxies or retained within the ICM less efficiently in lower mass systems. We explore possible causes, including variations in galaxy formation and metal release efficiency, cooling out of metals, and gas and metal loss via active galactic nuclei (AGN) – or starburst‐driven galactic winds from groups or their precursor filaments. Loss of enriched material from filaments coupled with post‐collapse AGN feedback emerges as viable explanations, but we also find evidence for metals to have been released less efficiently from galaxies in cooler groups and for the ICM in these to appear chemically less evolved, possibly reflecting more extended star formation histories in less massive systems. Some implications for the hierarchical growth of clusters from groups are briefly discussed.

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Section: Origin and Fate Of Icm Metals In Groupsmentioning

confidence: 95%

Temperature and abundance profiles of hot gas in galaxy groups - II. Implications for feedback and ICM enrichment

Rasmussen

Ponman

2009

Monthly Notices of the Royal Astronomical Society

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“…While there is evidence that rampressure stripping has produced H i deficiencies in galaxy groups with X-ray emitting IGM (e.g. Davis et al 1997;Sengupta & Balasubramanyam 2006), several studies concur that for galaxies with M * similar to NGC 90 (whether in galaxy groups or galaxy clusters), large offsets of their highest density H i beyond optical disk cannot be attributed to ram pressure alone (Bravo-Alfaro et al 2000;Chung et al 2009;Scott et al 2010). Still, we also note that the extent of the NGC 90 H i disk (assuming it is traced by the low-velocity H i component) is similar to that of its optical disk.…”

Section: Intra-group Medium and Ram Pressurementioning

confidence: 99%

Arp 65 interaction debris: massive H I displacement and star formation

Sengupta

Scott

Paudel

et al. 2015

A&A

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Context. Pre-merger tidal interactions between pairs of galaxies are known to induce significant changes in the morphologies and kinematics of the stellar and interstellar medium components. Large amounts of gas and stars are often found to be disturbed or displaced as tidal debris. This debris then evolves, sometimes forming stars and occasionally forming tidal dwarf galaxies. Here we present results from our H i study of Arp 65, an interacting pair hosting extended H i tidal debris.Aims. In an effort to understand the evolution of tidal debris produced by interacting pairs of galaxies, including in situ star and tidal dwarf galaxy formation, we are mapping H i in a sample of interacting galaxy pairs. The Arp 65 pair is the latest member of this sample to be mapped. Methods.Our resolved H i 21 cm line survey is being carried out using the Giant Metrewave Radio Telescope. We used our H i survey data as well as available SDSS optical, Spitzer infra-red and GALEX UV data to study the evolution of the tidal debris and the correlation of H i with the star-forming regions within it.Results. In Arp 65 we see a high impact pre-merger tidal interaction involving a pair of massive galaxies (NGC 90 and NGC 93) that have a stellar mass ratio of ∼1:3. The interaction, which probably occurred ∼1.0-2.5 × 10 8 yr ago, appears to have displaced a large fraction of the H i in NGC 90 (including the highest column density H i) beyond its optical disk. We also find extended on-going star formation in the outer disk of NGC 90. In the major star-forming regions, we find the H i column densities to be ∼4.7 × 10 20 cm −2 or lower. But no signature of star formation was found in the highest column density H i debris SE of NGC 90. This indicates conditions within the highest density H i debris remain hostile to star formation and it reaffirms that high H i column densities may be a necessary but not sufficient criterion for star formation.

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“…The morphology appears undistorted although there is evidence of multiple arms. IC 1933 is classified as "Sd" by Sengupta & Balasubramanyam (2006). The galaxy in both UV bands appears flocculent without a clear spiral arm structure.…”

Section: Uv Morphologymentioning

confidence: 99%

Galaxy evolution in Local Group analogs

Marino

Bianchi

Rampazzo

et al. 2010

A&A

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Context. Understanding the astrophysical processes acting within galaxy groups and their effects on the evolution of the galaxy population is one of the crucial topics of modern cosmology, as almost 60% of galaxies in the Local Universe are found in groups. Aims. We aim at learning about galaxy evolution within nearby groups dominated by late-type galaxies, specifically by studying their ultraviolet-emitting stellar population. Methods. We imaged in the far (FUV, λ eff = 1539 Å) and near ultraviolet (NUV, λ eff = 2316 Å) with the Galaxy Evolution Explorer (GALEX) three nearby groups, namely LGG 93, LGG 127 and LGG 225. We obtained the UV galaxy surface photometry and, for LGG 225, the only group covered by the SDSS, the photometry in u, g, r, i, z bands. We discuss galaxy morphologies looking for interaction signatures and we analyze the spectral energy distribution of galaxies to infer their luminosity-weighted ages. The UV and optical photometry was also used to perform a luminosity-weighted kinematical and dynamical analysis of each group and to evaluate the stellar mass. Results. A few member galaxies in LGG 225 show a distorted UV morphology due to ongoing interactions. (FUV − NUV) colors suggest that spirals in LGG 93 and LGG 225 host stellar populations in their outskirts younger than that of M 31 and M 33 in the Local Group or with less extinction. The irregular interacting galaxy NGC 3447A has a significantly younger stellar population (a few Myr old) than the average of the other irregular galaxies in LGG 225 suggesting that the encounter triggered star formation. The early-type members of LGG 225, NGC 3457 and NGC 3522, have masses of the order of a few 10 9 M , comparable to the Local Group ellipticals. For the most massive spiral in LGG 225, we estimate a stellar mass of ≈4 × 10 10 M , comparable to M 33 in the Local Group. Ages of stellar populations range from a few to ≈7 Gyr for the galaxies in LGG 225. The kinematical and dynamical analysis indicates that LGG 127 and LGG 225 are in a pre-virial collapse phase, i.e. still undergoing dynamical relaxation, while LGG 93 is likely virialized. Both the photometric and the dynamical analyses suggest that LGG 225 is in a more active evolution phase than LGG 93 and LGG 127.

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H i content in galaxies in loose groups

Cited by 51 publications

References 37 publications

Temperature and abundance profiles of hot gas in galaxy groups - II. Implications for feedback and ICM enrichment

Temperature and abundance profiles of hot gas in galaxy groups - II. Implications for feedback and ICM enrichment

Arp 65 interaction debris: massive H I displacement and star formation

Galaxy evolution in Local Group analogs

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