The H I Content of Spirals. II. Gas Deficiency in Cluster Galaxies

By J. Solanes, A. Manrique, C. García-Gómez, G. González‐Casado, R. Giovanelli, M. Haynes. 2000

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We derive the atomic hydrogen content for a total of 1900 spirals in the fields of 18 nearby clusters. By comparing the H I-deficiency distributions of the galaxies inside and outside one Abell radius (RA) of each cluster, we find that two-thirds of the clusters in our sample show a dearth of neutral gas in their interiors. Possible connections between the gaseous deficiency and the characteristics of both the underlying galaxies and their environment are investigated in order to gain insight into the mechanisms responsible for H I depletion. While we do not find a statistically significant variation of the fraction of H I-deficient spirals in a cluster with its global properties, a number of correlations emerge that argue in favor of the interplay between spiral disks and their environment. In the clusters in which neutral gas deficiency is pronounced, we see clear indications that the degree of H I depletion is related to the morphology of the galaxies and not to their optical size; early-type and probably dwarf spirals are more easily emptied of gas than the intermediate Sbc-Sc types. Gas contents below 1/10, and even 1/100, of the expectation value have been measured, implying that gas removal is very efficient. The radial extent of the region with significant gas ablation can reach up to 2RA. Within this zone, the proportion of gas-poor spirals increases continuously toward the cluster center. The wealth of 21 cm data collected for the Virgo region has made it possible to study the two-dimensional pattern of H I deficiency in that cluster. The map of gas deficiency in the Virgo central area points to an scenario in which gas losses result from the interaction of the disks with the inner hot intracluster gas around M87. We also find evidence that gas-poor spirals in H I-deficient clusters move in orbits more radial than those of the gas-rich objects. The implications of all these results on models of how galaxies interact with their environment are reviewed. Hydrodynamic effects appear as the most plausible cause of H I removal.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/2283c4244daf37cfb35df4a55c1edcaee8201475

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Citations in the corpus

VLA IMAGING OF VIRGO SPIRALS IN ATOMIC GAS (VIVA). I. THE ATLAS AND THE H i PROPERTIES (2009, background): “More recently, in a study of 18 nearby clusters, Solanes et al. (2001) show that the H i deficiency decreases gradually with an increasing projected distance from the cluster center out to ∼2 Abell radii (≈3 h−1 Mpc).”
The 2dF Galaxy Redshift Survey: The environmental dependence of galaxy star formation rates near clusters (2002, background): “…devoted to the study of galaxies in the cores of rich clusters, which differ so dramatically from more common galaxies (e.g. Dressler 1980; Dressler et al. 1985; Couch & Sharples 1987; Balogh et al. 1997, 1999; Poggianti et al. 1999; Moss & Whittle 2000; Couch et al. 2001; Solanes et al. 2001).”
Galaxy ecology: groups and low-density environments in the SDSS and 2dFGRS (2003, background): “Furthermore, the existence in clusters of HI-deficient spirals (e.g Solanes et al. 2001), red, spiral galaxies with little star-formation (e.g. Poggianti et al. 1999; Balogh et al. 2002a) and spiral galaxies with unusually smooth structure (McIntosh et al. 2003) all argue for”
A DOZEN NEW GALAXIES CAUGHT IN THE ACT: GAS STRIPPING AND EXTENDED EMISSION LINE REGIONS IN THE COMA CLUSTER (2010, background): “It is well known that galaxies residing in the central region of clusters are generally deficient in gas(e.g., Giovanelli & Haynes 1985; Gavazzi 1987; Solanes et al. 2001; Boselli & Gavazzi 2006; BravoAlfaro et al. 2009).”
VLA H I Observations of Gas Stripping in the Virgo Cluster Spiral NGC 4522 (2004, background): “Since many HI-deficient galaxies in clusters have highly radial orbits (Dressler 1986; Solanes et al. 2001), the ram pressure can vary by factors of 20-100 during the orbit (Vollmer etal 2001).”
The evolution of substructure - III. The outskirts of clusters (2004, unknown): “This is consistent with the findings of Solanes et al. (2001) who found evidence that gas-poor spirals in HI deficient clusters move in orbits more radial than those of the gas-rich objects.”
Virgo Galaxies with Long One-sided H I Tails (2007, background): “For example Solanes et al. (2001) find that gas deficiency gradually decreases out to two Abell radii from the cluster center and Lewis et al. (2002) and Gomez et al. (2003) find that the star formation rate depends on local galaxy density.”
Ram pressure stripping the hot gaseous haloes of galaxies in groups and clusters (2007, background): “…(e.g., Balogh et al. 2004; Hogg et al. 2004), star forming properties (e.g., Poggianti et al. 1999; Balogh et al. 2000; Gomez ⋆ E-mail: i.g.mccarthy@durham.ac.uk (IGM) et al. 2003), and the distribution and total mass of their gaseous component (e.g., Cayatte et al. 1994; Solanes et al. 2001).”
Environmental Effects on Late‐Type Galaxies in Nearby Clusters (2006, methodology): “After analyzing the H i properties of ∼1900 galaxies in 18 nearby clusters, Solanes et al. (2001) concluded that two-thirds of the clusters are composed of H i–deficient galaxies inside the Abell radius .”
Pre-Processing of Galaxies before Entering a Cluster (2003, background): “…fact, disk galaxies with a deficit of cold gas or a morphological sign of gas removal are often observed near cluster centers (Cayatte et al. 1990; Vollmer et al. 2000; Bravo-Alfaro et al. 2000, 2001; Solanes et al. 2001; Bureau, Carignan 2002; Vollmer 2003; Sofue et al. 2003; Yoshida et al. 2004).”
The effect of the environment on the Hi scaling relations (2011, background): “…defined as the difference, in loga- galaxies are mainly/only present in very high-density environments (Giovanelli & Haynes 1985; Cayatte et al. 1990; Solanes et al. 2001; Boselli & Gavazzi 2009), providing strong constraints on the possible environmental mechanisms responsible for the quenching…”
The GALEX Arecibo SDSS Survey - VIII. Final data release. The effect of group environment on the gas content of massive galaxies (2013, methodology): “Galaxies in more massive clusters such as Coma have more extreme levels of Hi deficiency (Solanes et al. 2001).”
THE VELOCITY FUNCTION IN THE LOCAL ENVIRONMENT FROM ΛCDM AND ΛWDM CONSTRAINED SIMULATIONS (2009, background): “The HI sources detected by ALFALFA are typically associated with star forming disk galaxies, spirals in rich clusters are less likely to be detected since these galaxies might be HI deficient (Solanes et al. 2001).”
Ram pressure stripping of disk galaxies. From high to low density environments (2005, background): “They are more deficient near the cluster centre (Solanes et al. 2001), but deficient galaxies can be observed out to large distances (2 Abell radii) from the cluster centre (Solanes et al. 2001).”
The UV-Optical Color Magnitude Diagram. II. Physical Properties and Morphological Evolution On and Off of a Star-forming Sequence (2007, methodology): “First of all, we correct for a dependence on stellar mass rather than morphological type or the combination of morphological type and radius, as in Solanes et al. (2001).”
BUDHIES II: a phase-space view of H i gas stripping and star formation quenching in cluster galaxies (2015, result): “Measurements of HI-deficiencies in cluster galaxies at low z also show a significant environmental effect only out to ∼ 2R200 (Solanes et al. 2001), in agreement with our results.”