Contents

• VLA HI Imaging of the brightest spiral galaxies in Coma
• 1 Introduction
• 2 Observational results
• 3 Results for H I detected galaxies
• 4 The H I and the ICM in Coma
• 5 H I and radio continuum of PSB and active galaxies
• 6 Conclusions
• Appendix A
• References
• Online Material

A&A 379, 347-361 (2001)
DOI: 10.1051/0004-6361:20011242

VLA HI Imaging of the brightest spiral galaxies in Coma

II. The HI Atlas and deep continuum imaging of selected early type galaxies

H. Bravo-Alfaro¹ - V. Cayatte² - J. H. van Gorkom³ - C. Balkowski²

1 - Departamento de Astronomía, Universidad de Guanajuato. Apdo. Postal 144, Guanajuato 36000, México
2 - Observatoire de Paris DAEC, and UMR 8631, associé au CNRS et à l'Université Paris 7, 92195 Meudon Cedex, France
3 - Department of Astronomy, Columbia University, 550 W 120th Street, New York, NY 10027, USA

Received 11 July 2001 / Accepted 4 September 2001

Abstract
In the first paper of this series we used H I observations of the 19 brightest spirals in Coma to analyze the dynamical state of the cluster. In this paper we present the detailed H I distribution and kinematics of the spirals that were detected in H I, and radio continuum data for a sample of star forming and post starburst galaxies in Coma. We discuss the importance of ICM-ISM interactions to explain the observed H I morphology. A rough comparison of observed H I sizes with predicted H I sizes from simulations by Abadi et al. (1999) gives reasonable agreement. We use the results on radio continuum emission to estimate the star formation rate in the PSB galaxies we pointed at. The radio continuum emission in the 11 so called post starburst galaxies, identified by Caldwell et al. (1993) in the cluster, is weak. Eight of the 11 were not detected down to a 3 sigma upper limit of 0.6 mJy. This sets an upper limit to the star formation rate in these galaxies of less than 0.2 $M_{\odot}$yr^-1. The three detected post starburst galaxies have a star formation rate of less than one solar mass per year. Thus none of the post starburst galaxies in Coma are dust enshrouded starbursts.

Key words: galaxies: clusters: individual: Coma - radio lines: galaxies

1 Introduction

This is our second paper on the imaging of the neutral hydrogen component as a tracer of environmental effects on galaxies in the Coma cluster. Global properties of Coma related with its dynamical state, as derived from our VLA 21 cm line survey, have been discussed in a previous paper (Bravo-Alfaro et al. 2000, hereafter referred to as Paper I). In the present work we give a complete catalogue of H I maps, channel maps, and velocity fields (for cases with sufficient resolution) for 19 detected galaxies. We compare the detailed H I distribution and kinematics with model predictions for the fate of H I in galaxies in a cluster environment. We pay particular attention to a class of so called starburst (SB) and post starburst (PSB) galaxies identified by Caldwell et al. (1993, C93 throughout this paper). For these galaxies we derive star formation rates (SFR) from the radio continuum emission and discuss the implications of current gas content and star formation rate on the evolution of the galaxies.

Several physical mechanisms have been proposed to play a major role affecting the evolution of galaxies in clusters; these processes can be classified according to three types: (a) interactions between the ICM and the interstellar medium (Gunn & Gott 1972; Nulsen 1982; Kenney & Young 1989), (b) interactions with the cluster gravitational field (e.g. Bekki 1999), and (c) galaxy-galaxy interactions (see Icke 1985; Lavery & Henry 1994; Moore et al. 1996, 1999). In many cases more than one of these processes will be at work, but which mechanism dominates under specific physical conditions and how it depends on the galaxy trajectory through the cluster is still a matter of debate. For instance Solanes et al. (2000) conclude from an observational study of eighteen clusters that ICM-ISM interactions are most important to explain the observed H I deficiency. In contrast, Moore et al. (1999) suggest in a numerical study that, in combination with ram-pressure stripping, galaxy harassment may convert disk galaxies into S0s. In spite of this debate, the fact that spirals in the central region of clusters like Virgo show smaller H I than optical disks (Warmels 1988; Cayatte et al. 1990, 1994), is unquestionably associated with the interaction with the ICM. These studies demonstrate the importance of detailed H I imaging of individual galaxies in clusters with a range of ICM conditions to assess what gas removal processes are at work.

Another fundamental process linked with the evolution of galaxies in clusters is the triggering and stopping of bursts of star formation (van den Bergh et al. 1990). As the ISM is the raw material from which stars form, the evolution of H I deficient galaxies and their star formation properties are undoubtedly affected by the interaction with the environment. From statistical analyses on large scales the SFR is known to decrease with increasing density (Dressler et al. 1999), whereas at smaller scales the ICM may produce significant enhancements to the star formation activity in individual galaxies, as shown in clusters like A1367 (Gavazzi et al. 1995) and Coma (Bothun & Dressler 1986). Recent work supports different scenarios: (1) On the theoretical side, Bekki (1999) concludes that the tidal gravitational field of a group-cluster merger may trigger a burst of star formation, accounting for the PSB population in clusters like Coma, while Vollmer et al. (2001b) suggest that local enhancement of star formation could be due to re-accretion of gas clouds after a ram pressure stripping event. (2) Observationally, Dressler et al. (1999) find a trend in the position of SB and PSB galaxies around the cluster, making the hot gas environment the best explanation for this phenomenon (see also Poggianti et al. 1999). From a study of spectroscopically selected post starburst galaxies, which turned out to be mostly located in the field, Zabludoff et al. (1996) conclude that in those more isolated galaxies the post starburst phenomenon is most likely caused by galaxy interactions and mergers.

In this paper we give the atlas of our VLA H I imaging of spirals in Coma, showing that the scenario depicted by the neutral hydrogen constitutes strong evidence in favor of ICM-ISM interaction to explain the H I morphologies and the star formation histories in the cluster. We also present results on the radio continuum emission obtained as a byproduct of the spectral line observations. These results are used to derive the star formation rate in the so called post starburst galaxies to explore the possibility that these are in fact dust enshrouded starbursts as has recently been suggested by Smail et al. (1999) for the intermediate redshift cluster CL0939+4713 (see also Miller & Owen 2001).

We organize the paper as follows. In Sect. 2 we review the observations. In Sect. 3 we describe H I observational results of individual detected galaxies, in Sect. 4 we discuss the role of ram pressure affecting galaxies in Coma, and compare H I observations with numerical simulations of ram pressure stripping by Abadi et al. (1999) and Vollmer et al. (2001b). In Sect. 5 we discuss the PSB galaxies; we compare our H I mass limits and current star formation rates based on the continuum with those of the more vigorously star forming galaxies and discuss the implications. The results are summarized in Sect. 6. In Appendix A, available in electronic form, we give the complete catalogue of H I channel maps. Throughout the paper we assume a distance of 70 Mpc to the Coma cluster (with H₀=100 kms^-1Mpc^-1), where an angular size of 1 arcmin corresponds to a linear size of ${\sim}$20 kpc.

2 Observational results

Our data consist of 21 cm line data obtained with the VLA. Twelve fields within one Abell radius of the Coma cluster (equivalent to 1.2$^{\circ}$) were observed with the VLA in its C configuration, and two of them reobserved in D configuration. The observed fields and the distribution of the 19 galaxies detected in H I around the cluster are shown in Paper I (Figs. 1 and 2). Most of the fields are devoted to the center of Coma and the regions where SB and PSB galaxies had been reported from optical observations. Our velocity resolution is 21 kms^-1, and 43 kms^-1 for some of the galaxies observed in both C and D configurations. The angular resolution ranges between 20 and 35 arcsec. The rms in the final cubes is between 0.35 and 0.40 mJy beam^-1, except in those fields observed in both C and D configurations, reaching rms values as low as 0.20 mJy beam^-1. Most of the channel maps shown in the Appendix (electronic version) are smoothed in velocity. More details on the H I observations are given in Paper I.

Eight out of the 19 detected galaxies are projected within 0.5 Mpc from the cluster center (we consider the position of the cD NGC4874 as the Coma center). These central galaxies lie inside or near the hot ICM as traced by the ROSAT X-ray emission (Briel et al. 1992; Vikhlinin et al. 1997), and most of them are very H I deficient. The H I deficiency is measured following Giovanelli & Haynes (1985), comparing the observed H I mass with the expected H I mass of an equivalent isolated spiral. Several galaxies detected in H I near the center of Coma show H I truncated disks as well as offsets between the optical and H I distributions (see Sect. 3). In a few cases unexpected differences between optical and H I velocities are found. Six of the galaxies detected in H I are reported by Bothun & Dressler (1986) as having blue disks; five of these are projected inside or near the cluster X-ray emission. None of the PSB galaxies reported by Caldwell et al. (1993, 1997) were detected in H I; we obtain for some of them H I mass upper limits down to $3 \times 10^7~$$M_{\odot}$.

Our radio continuum images are obtained as a byproduct of the H I observations. The images are built by averaging a set of those line free channels in a given cube. All of the H I detected spirals (except NGC4907) are also detected in the continuum with flux densities ranging between 2 and 16 mJy (see Paper I).

3 Results for H I detected galaxies

In this section we briefly describe the H I morphology of detected galaxies, and the remarkable features concerning galaxy dynamics as revealed by the H I.

IC3913, KUG1255+275, and Mrk057

These three galaxies were detected in the SW of Coma, between 17$^{\prime}$ and 25$^{\prime}$ south of the cD galaxy NGC4839. They display several common features: they are H I rich galaxies with regular gas distributions, where H I disks extend well beyond the optical (Figs. 1a, 2 and 3a).

Figure 1a: H I density distribution of IC 3913, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.3, 2.7, 4.0, and $5.4 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.7^{\prime \prime } \times 27.2 ^{\prime \prime }$.

Figure 1b: Intensity weighted mean velocity field of IC 3913. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $30.7^{\prime \prime } \times 27.2 ^{\prime \prime }$.

Figure 2: H I density distribution of KUG 1255+275, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 0.8, 1.4, 2.0, and $2.6 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.7^{\prime \prime } \times 27.2 ^{\prime \prime }$.

Figure 3a: H I density distribution of Mrk 057, superposed on a DSS B-band gray scale image. The contours are 0.6 (2.5 $\sigma$), 2.3, 3.4, 4.6, 5.7, 6.8 and $8.0 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.7^{\prime \prime } \times 27.2 ^{\prime \prime }$.

Figure 3b: Intensity weighted mean velocity field of Mrk 057. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $30.7^{\prime \prime } \times 27.2 ^{\prime \prime }$.

Systemic velocities for these galaxies are between 7400 km s^-1 and 7650 km s^-1, close to the value of the NGC4839 group, 7339 km s^-1 (Colless & Dunn 1996). Because of their position, lying far from the cluster center and outside the X-ray emission, no strong interaction with the ICM is expected. Although these three galaxies are likely to be part of the infalling NGC4839 group (Neumann et al. 2001), we see no signs of a gravitational interaction either optically or in H I or the radio emission. Velocity fields of IC3913 and Mrk057 are shown in Figs. 1b and 3b respectively.

NGC4848

This Scd galaxy is one of the most interesting objects in our sample. NGC4848 is a blue disk galaxy showing a very intriguing H I distribution (see Fig. 4),

Figure 4: H I density distribution of NGC 4848, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.0, 1.7, and $2.3 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.5^{\prime \prime } \times 27.5 ^{\prime \prime }$.

as we only detect gas in the northern edge of the galaxy, 19 $^{\prime\prime}$ (6.5 kpc) NW from the optical center. We are probably missing some H I flux previously detected by single dish observations in the center of the galaxy (Gavazzi 1989). This object was also observed in H${\alpha}$ by Amram et al. (1992) who reported a double peak in the H${\alpha}$ profile, with the northern H${\alpha}$ peak at the same position than the H I. Interestingly, the brightest HII regions are in the south, where the H I gas has been totally depleted. The star forming activity is also evidenced by 20 cm radio continuum emission above a level of 16 mJy. This emission shows an elongation to the NW which is resolved by the VLA FIRST Survey in two separated sources, one coincident with the optical center of NGC4848 and a secondary peak 12 $^{\prime\prime}$ NW, roughly at the same position than the H I. The CO imaging carried out by Vollmer et al. (2001a) shows the maximum of the emission coincident with the optical galaxy center and with the empty H I zone. A secondary CO peak is detected in the NW, roughly coincident with the H I and radio continuum emission. Lavezzi et al. (1999) reported a normal $M_{\rm H2}$ content ( $2.56 \times 10^9$ $M_{\odot}$), which gives a very low fraction of neutral to molecular gas ratio: $M_{\rm HI}$/ $M_{\rm H2}$ ${\sim}$ 0.17 (NGC4848 is H I deficient by a factor of around 10).

Mergers do not account for the H I morphology or the star formation activity in NGC4848, because no obvious companion is seen in the DSS optical image (Fig. 4). However, the more detailed B-band CCD imaging by Gavazzi et al. (1990) shows a ring-like structure and blue bright zones in the NW, where the H I and the secondary peaks of CO, H${\alpha}$ and 20 cm radio continuum are found. The hypothesis of a dwarf system crossing the NGC 4848 disk is explored by Vollmer et al. (2001a) but further observations, both optical and higher resolution H I imaging, are needed to confirm it. N-body simulations by the same authors suggest that NGC4848 has already gone through the cluster core, 4$\times$10⁸ yr ago, and is now moving away from the cluster. They conclude that re-accretion of some of the stripped gas could explain the star formation burst.

Mrk58

This Sb, blue disk galaxy is projected onto the X-ray emission, some 20$^{\prime}$ (${\sim}$400 kpc) SW of NGC4874, in the zone lying between the main cluster and the SW group. It is gas deficient by a factor of 3. Its H I map (Fig. 5) displays a considerably asymmetry,

Figure 5: H I density distribution of Mrk 058, superposed on a DSS B-band gray scale image. The contours are 0.2 (2.5 $\sigma$), 0.7, and $1.1 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.3^{\prime \prime } \times 27.6 ^{\prime \prime }$.

with the gas swept from the NE. The H I is observed at an offset position of ${\sim}$12 $^{\prime\prime}$(4 kpc) SW from the optical disk. The observed H I distribution could be explained if we consider the supersonic velocity of Mrk58 relative to the cluster, 1575 km s^-1 (the sound speed in Coma is estimated around 1460 km s^-1 by Stevens et al. 1999); under these conditions the interaction with the ICM may produce ram pressure stripping to enhance the density behind the galaxy (Stevens et al. 1999).

CGCG160-058 and CGCG160-076

These late-type spiral galaxies lie in the nearby northern vicinity of Coma, outside the X-ray emission. They are H I rich galaxies displaying regular gas distributions (Figs. 6a and 7a). As expected, considering their position relative to the cluster, no strong environmental effects are seen: their H I disks are larger than the optical, and the H I and optical centroids are coincident. Velocity fields are given in Figs. 6b and 7b.

CGCG160-086

Figure 6a: H I density distribution of CGCG 160-058, superposed on a DSS B-band gray scale image. The contours are 0.4 (2.5 $\sigma$), 1.6, 3.2, 6.4, and $9.6 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.5^{\prime \prime } \times 27.5 ^{\prime \prime }$.

Figure 6b: Intensity weighted mean velocity field of CGCG 160-058. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $30.5^{\prime \prime } \times 27.5 ^{\prime \prime }$.

Figure 7a: H I density distribution of CGCG 160-076, superposed on a DSS B-band gray scale image. The contours are 0.2 (2.5 $\sigma$), 0.8, 1.6, 3.3, 6.6 and $9.9 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $29.9^{\prime \prime } \times 26.9^{\prime \prime }$.

Figure 7b: Intensity weighted mean velocity field of CGCG 160-076. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $29.9^{\prime \prime } \times 26.9^{\prime \prime }$.

This Sb, blue disk galaxy, projected onto the SE outskirts of the X-ray emission drawn by ROSAT, was only marginally detected in the present survey. The galaxy is not resolved in H I, as shown in Fig. 8.

Figure 8: H I density distribution of CGCG 160-086, superposed on a DSS B-band gray scale image. The contours are 0.4 (2.5 $\sigma$), 0.9, and $1.3 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $35.2^{\prime \prime } \times 33.0 ^{\prime \prime }$.

We report an H I deficiency by a factor of ${\sim}$3, the H I disk appearing truncated in its periphery, but the low resolution does not allow to get a more conclusive picture.

IC 4040

This Sdm blue disk galaxy is projected near the very center of Coma, at only 15$^{\prime}$ (300 kpc) NE from NGC4874. Its H I distribution (see Fig. 9a) shows the H I contours compressed in the NW,

Figure 9a: H I density distribution of IC 4040, superposed on a DSS B-band gray scale image. The contours are 0.2 (5$\sigma$), 0.4, 0.7, 1.1, and $1.4 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $35.5^{\prime \prime } \times 34.1 ^{\prime \prime }$.

Figure 9b: Intensity weighted mean velocity field of IC 4040. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $35.5^{\prime \prime } \times 34.1 ^{\prime \prime }$.

and an offset in position of 9 $^{\prime\prime}$ (${\sim}$3 kpc), with the H I emission SE of the optical galaxy. Our detection confirms the double peak detection reported by Gavazzi (1989) at 7600 km s^-1 and 7850 km s^-1. The velocity field for this galaxy is shown in Fig. 9b.

NGC4907

This Sb galaxy was only marginally detected in H I (Fig. 10).

Figure 10: H I density distribution of NGC 4907, superposed on a DSS B-band gray scale image. The contours are 0.2 (2.5 $\sigma$), 0.5, and $0.9 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $39.8^{\prime \prime } \times 34.5 ^{\prime \prime }$.

It is H I deficient by a factor of ten and presents a shrunken H I disk (not resolved by the VLA beam) which is smaller than the optical disk. Two facts make an ICM-ISM interaction the most likely explanation for this picture: the high radial velocity relative to the cluster ( $v_{\rm rel}=1179$ km s^-1), and the projected location of NGC4907, which puts it in a very high density region, 20$^{\prime}$ (400 kpc) NE from the cluster center.

KUG1258+287, FOCA195 and CGCG160-098

Figure 11a: H I density distribution of KUG 1258+287, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.1, 2.2, 4.5, 6.8, and $9.0 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.2^{\prime \prime } \times 26.7 ^{\prime \prime }$.

Figure 11b: Intensity weighted mean velocity field of KUG 1258+287. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $30.2^{\prime \prime } \times 26.7 ^{\prime \prime }$.

Figure 12a: H I density distribution of FOCA 0195, superposed on a DSS B-band gray scale image. The contours are 0.2 (2.5 $\sigma$), 0.9, 1.8, 2.6, 3.5, and $4.4 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.2^{\prime \prime } \times 26.7 ^{\prime \prime }$.

Figure 12b: Intensity weighted mean velocity field of FOCA 0195. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $30.2^{\prime \prime } \times 26.7 ^{\prime \prime }$.

Figure 13a: H I density distribution of CGCG 160-098, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.1, 2.2, and $4.4 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $30.2^{\prime \prime } \times 26.7 ^{\prime \prime }$.

Figure 13b: Intensity weighted mean velocity field of CGCG 160-098. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $30.2^{\prime \prime } \times 26.7 ^{\prime \prime }$.

These objects are part of a group dominated by CGCG160-098 (see Biviano et al. 1996). As all the galaxies in Coma detected in H I outside the X-ray emission, this group shows a normal H I content and a regular gas distribution (Figs. 11a, 12a and 13a), with the H I more extended than the optical disk and coinciding with the optical position. Particular features of these galaxies are their systematic blue $m_{\rm UV}{-}b$ color (see Table 2 and Fig. 7 in Paper I), and their high radial velocity (between 8400 km s^-1 and 8880 km s^-1), indicating a fast accretion of the group towards the main cluster body. Normal rotation patterns are shown by the bluest objects KUG1258+287 and FOCA195 (see Figs. 11b and 12b). H I emission equivalent to $2.2 \times 10^{8}$ $M_{\odot}$ was detected at 1.4$^{\prime}$ W of KUG1258+287 but no optical counterpart is observed.

NGC4911

This is one of the two brightest spirals in Coma. The H I morphology of NGC4911 shows a shrunken disk with two central peaks and a normal surface density in the central region as predicted by ram-pressure stripping (Fig. 14a).

Figure 14a: H I density distribution of NGC 4911, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.4, and $2.0 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $29.8^{\prime \prime } \times 27.7^{\prime \prime }$.

Figure 14b: Intensity weighted mean velocity field of NGC 4911. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $29.8^{\prime \prime } \times 27.7^{\prime \prime }$.

A shift in position is shown between the H I and the optical, the former lying about 4 kpc south of the optical component. NGC4911 shows a very high total gas content, $M_{\rm HI}$ + $M_{\rm H2}$ ${\sim}$ $3.7 \times 10^9$ $M_{\odot}$ (Casoli et al. 1996), but only a small fraction ( $M_{\rm HI}$/ $M_{\rm H2}$ = 0.34) is in atomic form. Considering the CO observations by Lavezzi et al. (1999) this fraction is much lower: $M_{\rm HI}$/ $M_{\rm H2}$ = 0.22. The velocity field shows normal rotation of the inner disk (see Fig. 14b) along an axis oriented roughly SE-NW.

NGC4911, projected 20$^{\prime}$SE of NGC4874 ( $v_{\rm rel}$ ${\sim}$ 1000 km s^-1), is thought to be the dominant galaxy of a group that recently crossed the cluster core (Biviano et al. 1996). Vikhlinin et al. (1997) reported an X-ray filamentary structure in this region, crossing over NGC4911 and culminating at the position of NGC4921. This cool spot has recently been confirmed with XMM (Arnaud et al. 2001), who consider the possibility of gas stripped from an infalling group, but not directly produced in the Coma center. They found that part of the X-ray excess in this zone is due to NGC4911. No other galaxies of this group were detected in H I, in support of the stripping hypothesis. However, the fact that none of the 14 catalogued galaxies (Biviano et al. 1996) have been classified as spirals weakens this argument somewhat.

NGC4922

This is the best known case of a merger in Coma, and the only pair detected in this survey; it is located in the northern most field, 1.4$^{\circ}$ from the cluster center. It is very bright in radio (27.5 mJy) and the brightest IR source in Coma (Mirabel & Sanders 1988). NGC4922 consists of two merging galaxies, one spiral in the north and one early type galaxy in the south. We detected H I in emission and absorption. The H I shown in Fig. 15,

Figure 15: H I density distribution showing the emission feature of NGC 4922, superposed on a DSS B-band gray scale image. Strong H I absorption is present which attenuates the emission. The contours are 0.2 (2.5 $\sigma$), 0.4, and $0.5 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $57.8^{\prime \prime } \times 53.4^{\prime \prime }$.

centered in the spiral galaxy, is strongly attenuated by the absorption. An H I emission equivalent to $5.8 \times 10^{7}$ $M_{\odot}$ was detected south of the merging system, but no optical counterpart is evident from the DSS image.

NGC4921

This is the brightest spiral in Coma, located 24$^{\prime}$ (${\sim}$0.5 Mpc) SE from NGC4874. It roughly coincides with a second order X-ray peak (Vikhlinin et al. 1997) also detected with XMM by Arnaud et al. (2001) and Briel et al. (2001). NGC4921 presents a very peculiar picture in 21 cm: a double peaked H I disk (Fig. 16a) which is considerably smaller than the optical one,

Figure 16a: H I density distribution of NGC 4921, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.2, 1.7, and $2.3 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $39.8^{\prime \prime } \times 34.5 ^{\prime \prime }$.

Figure 16b: Intensity weighted mean velocity field of NGC 4921. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $39.8^{\prime \prime } \times 34.5 ^{\prime \prime }$.

with a strongly asymmetric distribution, with most of the neutral gas distributed along the SE spiral arm. The gaseous disk presents a striking shift in position of ${\sim}$25 $^{\prime\prime}$ (some 8 kpc) SE from the optical. The velocity field is shown in Fig. 16b.

NGC4921 is perhaps the best example in Coma where several mechanisms are present simultaneously. (a) The shrunken H I disk and the shift between optical and H I positions look like clear signatures of ram-pressure stripping, which is also supported by the supersonic velocity of the galaxy relative to the cluster, 1521 km s^-1. (b) NGC4921 shows the largest cross section in our sample, which could produce, by viscous stripping, a mass loss rate value up to 20 $M_{\odot}$yr^-1. Another feature supporting viscous stripping is the relatively low surface gas density in the central region of NGC4921, previously classified as anemic by van den Bergh (1976). (c) The NW zone, where the brightest HII regions are seen (Amram et al. 1992), appears depleted of H I, similar to the case of NGC4848. Furthermore, NGC4921 displays a high total gas content, $M_{\rm HI}$ + $M_{\rm H2}$ = $2.65 \times 10^9$ $M_{\odot}$, with only a small fraction (0.36) in atomic form, suggesting that H I is actively converted to molecular gas. Gas re-accretion in the NW may also be present, triggering the HII regions along the spiral arm. As this galaxy does not show any optical distortion, processes involving gravitational effects are unlikely to be important.

IC842 and IC4088

Figure 17a: H I density distribution of IC 842 superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.2, 2.5, 3.7, 4.9, 6.2, and $7.4 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $36.6^{\prime \prime } \times 35.4^{\prime \prime }$.

Figure 17b: Intensity weighted mean velocity field of IC 842. The optical center of the galaxy is indicated with a cross. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $36.6^{\prime \prime } \times 35.4^{\prime \prime }$.

Figure 18a: H I density distribution of IC 4088 and 3 neighbor dwarf systems, superposed on a DSS B-band gray scale image. The contours are 0.2 (2.5 $\sigma$), 1.0, 1.9, 2.9, 3.9, 5.8, 7.8, and $9.7 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $36.6^{\prime \prime } \times 35.4^{\prime \prime }$.

Figure 18b: Intensity weighted mean velocity field of IC 4088. The optical center of the galaxies are indicated with crosses. The numbers indicate heliocentric velocity in km s-1. The FWHM is indicated by the circle, $36.6^{\prime \prime } \times 35.4^{\prime \prime }$.

These galaxies lie in the far northern region of Coma, along the supercluster NE filament, and far from the X-ray emission. As expected, they display normal H I content and no effects of interaction with the ICM are seen (Figs. 17a and 18a). They also display normal rotation patterns (Figs. 17b and 18b). Three dwarf systems were detected in H I around IC4088, one of them ([GMP 83] 1866) lies at only 2$^{\prime}$ (${\sim}$40 kpc) north of the spiral, but no optical distortions are evident. The dwarfs show velocity dispersions between 43 km s^-1 and 173 km s^-1, and their H I masses range between 0.2 and $2.0 \times 10^9$ $M_{\odot}$. All the galaxies detected in this region, including the merger NGC4922, are likely part of a group falling towards to the cluster center (Paper I).

CGCG160-106

This blue disk galaxy is located in the SE outskirts of the X-ray emission. The ICM does not exert important effects on this galaxy because of the low ICM density at the galaxy position, the low value of $v_{\rm rel}$, and the small cross section. CGCG160-106 is not very H I poor (it is deficient by a factor of 1.5), and the H I morphology, barely resolved in Fig. 19,

Figure 19: H I density distribution of NGC 4926-A, superposed on a DSS B-band gray scale image. The contours are 0.3 (2.5 $\sigma$), 1.4, and $2.1 \times 10^{20}$ cm-2. The FWHM is indicated by the circle, $35.2^{\prime \prime } \times 33.0 ^{\prime \prime }$.

only shows a shrunken disk slightly bigger than the optical one.

We detect a clear shift in the H I position, lying 15 $^{\prime\prime}$ (some 5 kpc) SW from the optical disk, and an intriguing difference in velocity between the H I and optical: 6876 km s^-1 and 7188 km s^-1, respectively. Amram et al. (1992) observed this galaxy in H${\alpha}$ and reported a velocity of 7100 km s^-1 and an extension to the SW, coincident with the position of a dwarf companion separated by ${\sim}$20 $^{\prime\prime}$. We detect weak H I emission in the same zone, but higher resolution is needed to resolve the dwarf system.

4 The H I and the ICM in Coma

As mentioned earlier, physical mechanisms affecting galaxies in clusters are produced by interactions with one or more of the next three elements: the hot ICM, neighbor galaxies, and the cluster gravitational field. Two effects observed in H I in this work are explained on the basis of ICM-ISM interactions: the position of H I deficient galaxies relative to the ICM as drawn by the X-ray emission, and the fact that the most central galaxies detected in H I appear stripped in their outer regions, as predicted for ram-pressure stripping. If tidal interactions were predominant there should be evidence of optical signatures of the interaction, but none of the H I deficient galaxies in this work (except the merger NGC4922), neither detected nor undetected, display peculiarities in their optical morphology. It was also shown in Paper I that tidal interactions are unlikely to be the explanation for the disturbed H I disks in Coma or the triggering of starburst events, because there is no correlation between these effects and the number of close neighbors.

In order to confirm the role of ram pressure stripping in producing the observed H I distributions and in enhancing the star formation in Coma, it is fundamental to compare the H I imaging with 3D simulations of the ISM-ICM interaction. A thorough comparison will help to estimate the role played by different infalling orbits, inclination angles, and ICM densities, as well as to determine the stripping time scale and the regions of the disk where ram-pressure is more effective. To this aim we compare our H I observations with predictions made by 3D-simulations carried out by Abadi et al. (1999) and Vollmer et al. (2001b).

Simulations by Abadi et al. (1999) are a good point of departure even if the clumpiness of the ISM and different elapsed times after crossing the cluster core are not taken into account. They computed the expected radius of a ram pressure stripped gas disk ( $R_{\rm str}$) for a Coma cluster-like density and dispersion velocity. For instance, a typical galaxy in Coma with $v_{\rm rel}$ ${\sim}$ 1000 kms^-1 would have $R_{\rm str}$ ${\sim}$ 6kpc. In Table 1 we compare the observed H I radius (or upper limits if resolution is marginal) with the prediction of $R_{\rm str}$ made by Abadi et al. (1999). Columns 1 and 2 give the galaxy identification, Col. 3 gives the radial velocity relative to the cluster. In Col. 4 we give the observed H I radius in kpc estimated at a level of $3 \times 10^{19}$ $M_{\odot}$, taking the average between major and minor H I axis (none of the galaxies in Table 1 are very elongated). Column 5 gives the observed H I radii corrected for the beam; for galaxies marginally resolved (indicated with *) we give 0.5 times the beam size as an upper limit of the beam corrections, following Wild (1970). Column 6 gives the predicted value of $R_{\rm str}$ from Abadi et al. (1999), considering the corresponding velocity of the galaxy relative to the cluster.

 

 

Table 1: Comparison between the observed and predicted H I radius in kpc, for central galaxies in Coma.

CGCG	Other	$v_{\rm rel}$	Obs	Corr	Pred
	name	kms-1	$r_{{\rm HI}}$	$r_{{\rm HI}}$	$r_{{\rm HI}}$
(1)	(2)	(3)	(4)	(5)	(6)
160-055	NGC4848	41	6.8	5.0*	17.0
160-073	Mrk058	1575	7.9	5.8	4.5
160-086		481	6.0	5.6*	8.5
160-252	IC4040	758	10.2	8.0	7.5
160-257	NGC4907	1180	6.6	5.8*	5.5
160-260	NGC4911	997	12.7	12.2	6.5
160-095	NGC4921	1521	11.2	10.2	5.0
160-106	NGC4926-A	124	8.2	5.7	14.0

(*) Galaxies marginally resolved in H I.

The predicted H I radius is calculated assuming that the galaxy's distance to the center equals its projected distance and its velocity through the cluster equals its radial velocity. Considering those assumptions there is good agreement between observed and predicted values of the HI radius. The two galaxies (NGC4848 and 4926-A) that have significantly smaller radii than predicted must have a non negligible velocity in the plane of the sky, while the giants NGC 4911 and 4921 are probably at larger distance from the center and only in projection very close. For the three unresolved galaxies the H I distribution is limited to a central region of $\leq$6 kpc. Our results for H I deficient yet detected galaxies in Coma, confirm that most of the restoring force is coming from the central parts of the disk where the presence of the bulge is more important, as found by Abadi et al.'s simulation. They found that the gas is not completely removed by ram pressure, suggesting that other processes may be at work affecting those spirals which are not detected in H I in this survey.

Three dimensional simulations taking into account the clumpiness of the ISM were carried out for the Virgo cluster by Vollmer et al. (2001b). These authors found that stripping is very effective for galaxies that are on radial orbits through the cluster, in agreement with observational evidence provided by Dressler (1984) and Solanes et al. (2000). Vollmer et al. (2001b) found that time scales for ram pressure effects in Virgo may be as short as $3 \times 10^7$ yr, and in Coma they would likely be shorter because of its larger core size and more hostile ICM conditions. Interestingly, those authors found that galaxies showing important gas disruptions are not infalling but have already gone through the cluster core. If this is valid in Coma, it would confirm that all the central spirals (see Fig. 2 of Paper I) have already gone through the cluster core, while the H I regular galaxies in the outskirts of the X-ray emission are in the process of infalling (see Sect. 3). Some of the consequences in Coma are discussed in the next section.

 

 

Table 2: HI and radio continuum parameters of abnormal spectrum galaxies (top) and blue disks (bottom) in Coma.

ID	Other name	Morph.	$M_{\rm HI}$	$F_{{\rm cont}}$	rms noise	L1.4	SFR	SFR/$L_{\rm B}$
		type	108 $M_{\odot}$	mJy	mJy Beam-1	1020 WHz-1	$M_{\odot}$ yr-1	$M_{\odot}$(yr $L_{\odot})^{-1}$
(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)	(9)a
D 77	Leda 83676	S0/a (SB)	<0.6	-	0.18	<3.17	<0.19	<0.23
D 94	Leda 83682	SA0  (PSB)	<0.5	-	0.18	<3.17	<0.19	<0.17
D 112	Leda 83684	SB0  (PSB)	<0.4	-	0.18	<3.17	<0.19	<0.03
D 21	MCG 5-31-037	SBa  (PSB)	<0.7	-	0.19	<3.35	<0.20	<0.09
D 73	RB 183	SA0  (PSB)	<0.9	-	0.17	<3.00	<0.18	<0.27
D 44	KUG1256+278A	S0    (SB)	<0.6	-	0.18	<3.17	<0.19	<0.18
D 43	NGC 4853	SA0  (SB)	<0.5	1.2	0.18	7.06	0.42	0.06
D 89	IC 3949	SA0  (PSB)	<0.3	2.1	0.18	12.35	0.73	0.18
D 127	RB 042	S0    (PSB)	<0.6	1.0	0.18	5.88	0.35	0.46
D 216	RB 160	Sa    (PSB)	<0.7	-	0.18	<3.17	<0.19	<0.28
D 99	Mrk 060	SB0  (PSB)	<0.7	1.2	0.19	7.06	0.42	0.23
D 146	RB 110	S0    (PSB)	<0.3	-	0.18	<3.17	<0.19	<0.16
D 61	CGCG 160-104	SA0  (PSB)	<0.7	-	0.10	<1.76	<0.10	<0.03
D 189	Leda 83763	S0    (PSB)	<1.5	-	0.17	<3.00	<0.18	<0.31
160-055	NGC 4848	Scd	4.3	16.6	0.18	97.37	5.75	0.38
160-073	Mrk 058	Sb	2.0	5.5	0.17	32.10	1.89	0.56
160-086		Sb	1.7	3.8	0.15	22.11	1.30	0.88
160-252	IC 4040	Sdm	3.3	15.0	0.18	88.20	5.20	1.00
160-098		Sbc	7.3	5.7	0.18	33.34	1.97	0.62
160-106	NGC 4926-A	Sa	6.0	3.1	0.15	18.17	1.07	0.49

^a In units of 10^-9.

5 H I and radio continuum of PSB and active galaxies

The physical mechanisms which trigger and quench the star formation activity, and the question if the star burst exhausts the H I reservoir is still a matter of debate. We address this problem pointing at 14 galaxies in Coma for which abnormal spectra are reported by Caldwell et al. (1993, 1997), in order to get H I and radio continuum information. The radio continuum at 1.4 GHz could be due to synchrotron emission from relativistic electrons accelerated by supernovae hence probing star formation, or it could come from AGN. At intermediate redshift Smail et al. (1999) detect in the cluster CL0939+4713 (z=0.41) several post starburst galaxies in radio continuum and these authors argue that the PSBs are most likely dust enshrouded starbursts. In the local universe Chang et al. (2001) observed in H I five of the spectroscopically selected sample of E+A galaxies (Zabludoff et al. 1996). They detected one in H I  and none in radio continuum. The implied low star formation rates and limits on the SFR for these galaxies rule out that any of these is in fact a dust enshrouded starburst.

Eleven of the 14 abnormal spectrum galaxies we pointed at in Coma are defined as PSBs because of their spectra with strong absorption lines and no emission at all; the three remaining are star forming systems (SBs), as indicated by their emission line spectrum superposed to absorption lines (C93). Their position relative to the X-ray emission is shown in Paper I (Fig. 6). We detected none of these objects in H I, and report very low H I mass upper limits between 3 and $7 \times 10^{7}$ $M_{\odot}$ (see Table 2). We do detect weak radio continuum emission in three PSB (IC3949, Mrk060 and RB042) and one SB galaxy (NGC4853, see Table 2). Our radio continuum levels in Coma imply even lower limits to the star formation rates than found by Miller & Owen (2001) and Chang et al. (2001) for the field E+A's. Thus in Coma, contrary to in CL 0939+4713, the post starburst galaxies have at best only very modest levels of star formation. Chang et al. (2001) detected one of five E+A's in H I, while our H I upper limits for the cluster PSBs are almost two orders of magnitude below this detection. This may indicate a real difference between cluster and field post starburst galaxies. Whatever triggers the starburst, whether collisions or ICM interaction, in a cluster the gas is cleaned out after the starburst, something that would not happen in the field. We show that the post starburst galaxies in Coma have very little, if any, H I.

Table 2 gives in the upper part the H I mass upper limits and radio continuum parameters for the sample of abnormal spectrum galaxies that we observed. For comparison, we show in the bottom the same results for the blue disks. RB042 is projected very close to the cD galaxy NGC4874 and was only marginally detected in radio. Three of four galaxies are new detections, the fourth, NGC4853, is catalogued in the FIRST Survey (Becker et al. 1995). Table 2 gives in Cols. 1 and 2 the galaxy identification, Col. 3 gives the morphological and spectral classification, following C93. In Col. 4 we list the H I upper limits, in Col. 5 the radio continuum flux, Col. 6 lists the rms noise in the continuum images. In Col. 7 we give the radio power, with upper limits set at 3 sigma. The associated SFR, listed in Col. 8, is calculated following Yun et al. (2001): ${\it SFR}_{1.4}=L_{1.4}$[ $5.9 \times 10^{\rm -22}$ WHz^-1]$M_{\odot}$yr^-1. In Col. 9 we give the relation between the SFR and the blue luminosity ($L_{\rm B}$) obtained from the blue total magnitude, using the Mean Data from the LEDA database for homogeneity.

Table 2 shows that the SFR in the PSBs is well below 1 $M_{\odot}$yr^-1. It comes as somewhat of a surprise that also the SB galaxies have SFR less than 1 $M_{\odot}$yr^-1. This contrasts sharply with the blue disk galaxies reported by Bothun & Dressler (1986), which were all detected in continuum (see Table 2) and for which the associated SFR are from 1.0 to 5.5 $M_{\odot}$yr^-1. We note that these rates are in good agreement with the rates reported from the H${\alpha}$ equivalent widths by Bothun & Dressler (1986). Thus the blue "starforming" disks have a significantly higher SFR than the "starbursting" galaxies identified by C93. This is also valid if we consider the factor SFR/$L_{\rm B}$ given in Col. 9 of Table 2, which is probably a better criteria than merely SFR if the sampled galaxies span a large range in size and luminosity. There is a consistent trend between Cols. 8 and 9, with blue disks showing systematically higher values of SFR/$L_{\rm B}$ than galaxies from C93. The explanation is simple: C93 only selected early type galaxies for their sample of abnormal spectrum galaxies. The emission lines typically have narrow H$\delta$ lines ($\leq$3 ${\rm\AA}$), while the blue disks have 3 ${\rm\AA}$ $\leq$ H$\delta$ $\leq$ 7 ${\rm\AA}$. Thus the SB in the C93 sample means a higher than usual SFR for an early type galaxy; the absolute levels are very low. It is interesting that the C93 sample is spatially distinct from the blue disks. The latter are located at the edge of the X-ray emission, while most of the C93 galaxies are in the cluster core or in the zone between the core and the SW group. The difference in environment may well account for the different star formation properties of these galaxies.

HST images (Caldwell et al. 1999) show that some of the PSB galaxies in Coma have retained their disk, even with a smooth spiral structure. D61 (Zw 160-104) shows two dust lanes forming an edge-on disk, and D216 (RB 160) shows clear spiral structure. Interestingly our limits to the SFR and H I content for these two galaxies are very low. Obviously the time scale for gas removal from these galaxies was shorter than for a morphological transformation. Caldwell et al. (1999) suggest that star formation activity in the PSBs of Coma could be triggered by galaxy harassment and by gravitational perturbations between the main cluster and the SW group. However, Moore et al. (1996) estimate a time-scale of ${\sim}$3 Gyr to produce considerable changes in the optical morphology by this process. This is too long for galaxies like D61 and D216 to explain the whole process of triggering a starburst, the loss of a big fraction of their gas reservoir, and the subsequent quenching of the activity. An alternative process to explain this scenario is the re-accretion of gas mass after the stripping, as the infalling gas colliding with the clouds remaining in the disk can trigger star formation within the disk. In a cluster like Virgo this process starts at ${\sim}$ $2 \times 10^8$ years after the closest passage of the cluster core, and ends at ${\sim}$ $5 \times 10^8$ years (Vollmer et al. 2001b). The same process in Coma should develop with at least the same time-scales (or shorter, if we consider the more hostile ICM conditions), suggesting that the interaction with the ICM and gas re-accretion may account for this scenario. This is reinforced by the fact that galaxies could reach their present condition during a single pass through the cluster core, on a time scale $\leq$1 Gyr, which is much shorter than the time needed by galaxy harassment to modify the optical morphology. The cases of the PSBs D61 and D216 support this scenario: the former presents a very young starburst age of 0.5 Gyr, and the latter, recently reclassified as a spiral (Caldwell et al. 1999), should have harbored a significant amount of gas in the recent past. Both need a faster process than galaxy harassment to account for the sudden removal of the H I reservoir and quenching of star forming activity.

The gas which has been accelerated to values below the escape velocity will accrete back to the galaxy at time scales of 2- $7 \times 10^8$ years (Vollmer et al. 2001b). As a first approach in Coma we apply a conservative value of $5 \times 10^8$ years for the re-accretion time scale, i.e. the same value found by Vollmer et al. in Virgo. If we consider a typical galaxy moving across the Coma cluster at $v_{\rm rel}$ ${\sim}$ 1000 kms^-1 (equivalent to the velocity dispersion) it will travel some 0.5 Mpc before the gas accretes back on to the disk and triggers a burst of star formation. It is very interesting to associate this with the fact that a considerable fraction (38%) of the star forming UV flux in Coma is produced in an annular region between 20$^{\prime}$ and 30$^{\prime}$, or ${\sim}$0.5 Mpc from the cluster center (Donas et al. 1995), and that it is in this zone where most of the blue galaxies in Coma are located (Paper I). Taking into account their position relative to the cluster, NGC4848 and most of the blue disk galaxies in Coma have had enough time after passing across the cluster core to re-accrete gas clouds and boost a major star formation event; this mechanism may in part account for the blue annulus observed in Coma which is also observed in high redshift clusters (Oemler 1992).

6 Conclusions

In this paper we present the H I morphology and kinematics of the brightest spirals in Coma. We compare the H I morphology with numerical simulations on ram pressure stripping by the ICM. We derive star formation rates for a sample of post starburst and actively star forming galaxies, from deep continuum imaging obtained as a byproduct of the H I observations. We conclude that the H I morphology of the spirals in Coma, the location of the H I deficient galaxies and the size of the H I disks are consistent with predictions of the effect of ram pressure stripping by the ICM.

Targeted observations of 11 of the 14 known PSB galaxies in Coma give H I upper limits between 3 and $7 \times 10^{7}$ $M_{\odot}$ in H I. The star formation rates derived from (upper limits to) the radio continuum are less than 1 $M_{\odot}$yr^-1. Even the early type galaxies with abnormal emission lines (SB galaxies from Caldwell et al.) have SFR well below 1 $M_{\odot}$yr^-1. Thus in Coma there is no evidence for the presence of the dust enshrouded starburst galaxies, which may have been found in clusters at intermediate redshift. We found additional observational evidence confirming a real difference between cluster and field post starbursts; galaxies in clusters would exhaust the gas after the starburst, something that is not always observed in the field.

Acknowledgements

We are very grateful to E. Brinks for helping to improve this paper significantly. HBA thanks the DAEC of the Observatoire de Paris, the Astronomy Department of Columbia University, and the AOC of the NRAO, for support and hospitality during his visits. We used the Digital Sky Survey, produced at the Space Telescope Science Institute. We have made use of the Lyon-Meudon Extragalactic Database (LEDA) supplied by the LEDA team at the CRAL-Observatoire de Lyon (France). We used NED, the NASA/IPAC extragalactic database, operated for NASA by the Jet Propulsion Laboratory at Caltech. This work has in part been supported by NSF grant AST-97-17177 to Columbia University. We appreciate the suggestions done by an anonymous referee and the efficiency with which this paper passed through the whole evaluation procedure.

Appendix A

Individual Channel Maps (Presented in increasing Right Ascension Order) This appendix is only available in electronic form at http://www.edpsciences.org

References

 

• Abadi, M. G., Moore, B., & Bower, R. G. 1999, MNRAS, 308, 947 NASA ADS  
• Amram, P., Le Coarer, E., Marcelin, M., et al. 1992, A&AS, 94, 175 NASA ADS  
• Arnaud, M., Aghanim, N., Gastaud, R., et al. 2001, A&A, 365, L67 NASA ADS  
• Becker, R. H., White, R. L., & Helfand, D. J. 1995, ApJ, 450, 559 NASA ADS  
• Bekki, K. 1999, ApJ, 510, L15 NASA ADS  
• Biviano, A., Durret, F., Gerbal, D., et al. 1996, A&A, 311, 95 NASA ADS  
• Bothun, G., & Dressler, A. 1986, ApJ, 301, 57 NASA ADS  
• Bravo-Alfaro, H., Cayatte, V., van Gorkom, J. H., & Balkowski, C. 2000, AJ, 119, 580 (Paper I) NASA ADS  
• Briel, U. G., Henry, J. P., & Bohringer, H. 1992, A&A, 259, L31 NASA ADS  
• Briel, U. G., Henry, J. P., Lumb, D. H., et al. 2001, A&A, 365, L60 NASA ADS  
• Caldwell, N., Rose, J. A., Sharpless, R. M., Ellis, R. S., & Bower, R. G. 1993, AJ, 106, 473 NASA ADS  
• Caldwell, N., & Rose, J. A. 1997, AJ, 113, 492 NASA ADS  
• Caldwell, N., Rose, J. A., & Dendy, K. 1999, AJ, 117, 140 NASA ADS  
• Casoli, F., Dickey, J., Kazès, I., et al. 1996, A&AS, 116, 193 NASA ADS  
• Cayatte, V., van Gorkom, J. H., Balkowski, C., & Kotanyi, C. 1990, AJ, 100, 604 NASA ADS  
• Cayatte, V., Kotanyi, C., Balkowski, C., & van Gorkom, J. H. 1994, AJ, 107, 1003 NASA ADS  
• Chang, T., van Gorkom, J. H., Zabludoff, A.I., Zaritsky, D., & Mihos, C. 2001, AJ, 121, 1965 NASA ADS  
• Colless, M., & Dunn, A. M. 1996, ApJ, 458, 435 NASA ADS  
• Donas, J., Milliard, B., & Laget, M. 1995, A&A, 303, 661 NASA ADS  
• Dressler, A., Smail, I., Poggianti, B. M., et al. 1999, ApJS, 122, 51 NASA ADS  
• Dressler, A. 1984, ARA&A, 22, 185 NASA ADS  
• Gavazzi, G. 1989, ApJ, 346, 59 NASA ADS  
• Gavazzi, G., Garilli, B., & Boselli, A. 1990, A&AS, 83, 399 NASA ADS  
• Gavazzi, G., Contursi, A., Carrasco, L., et al. 1995, A&A, 304, 325 NASA ADS  
• Giovanelli, R., & Haynes, M. P. 1985, ApJ, 292, 404 NASA ADS  
• Gunn, J. E., & Gott, J. R. 1972, ApJ, 176, 1 NASA ADS  
• Icke, V. 1985, A&A, 144, 115 NASA ADS  
• Kenney, J. D. P., & Young, J. S. 1989, ApJ, 344, 171 NASA ADS  
• Lavery, R. J., & Henry, J. P. 1994, ApJ, 426, 524 NASA ADS  
• Lavezzi, T. E., Dickey, J. M., Casoli, F., & Kazès, I. 1999, ApJ, 117, 1995  
• Miller, N. A., & Owen, F. N. 2001, ApJ, 554, L25 NASA ADS  
• Mirabel, I. F., & Sanders, D. B. 1988, ApJ, 355, 104  
• Moore, B., Katz, N., Lake, G., Dressler, A., & Oemler, A. 1996, Nature, 379, 613 NASA ADS  
• Moore, B., Lake, G., Quinn, T., & Stadel, J. 1999, MNRAS, 304, 465 NASA ADS  
• Neumann, D. M., Arnaud, M., Gastaud, R., et al. 2001, A&A, 365, L74 NASA ADS  
• Nulsen, P. E. J. 1982, MNRAS, 198, 1007 NASA ADS  
• Oemler, A. 1992, in Clusters and Superclusters of Galaxies, ed. A. C. Fabian (Dordrecht:Kluwer), 29  
• Poggianti, B. M., Smail, I., Dressler, A., et al. 1999, ApJ, 518, 576 NASA ADS  
• Smail, I., Morrison, G., Gray, M. E., et al. 1999, ApJ, 525, 609 NASA ADS  
• Solanes, J. M., Manrique, A., García-Gómez, C., et al. 2001, ApJ, 548, 97 NASA ADS  
• Stevens, I. R., Acreman, D. M., & Ponman, T. J. 1999, MNRAS, 310, 663 NASA ADS  
• van den Bergh, S. 1976, ApJ, 206, 883 NASA ADS  
• van den Bergh, S., Pierce, M., & Tully, R. B. 1990, ApJ, 359, 4 NASA ADS  
• Vikhlinin, A., Forman, W., & Jones, C. 1997, ApJ, 474, L7 NASA ADS  
• Vollmer, B., Braine, J., Balkowski, C., Cayatte, V., & Duschl, W. J. 2001a, A&A, 374, 824 NASA ADS  
• Vollmer, B., Cayatte, V., Balkowski, C., Duschl, W. J. 2001b, ApJ, in press [astro-ph/0107237]  
• Warmels, R. H. 1988, A&AS, 72, 19 NASA ADS  
• Wild, J. P. 1970, Aust. J. Phys., 23, 113  
• Yun, M. S., Reddy, N. A., & Condon, J. J. 2001, ApJ, in press [astro-ph/0102154]  
• Zabludoff, A. I., Zaritsky, D., Lin, H., et al. 1996, ApJ, 466, 104 NASA ADS

 

Online Material

Figure A.1: The mosaic of the channel maps of IC 3913, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.7'' \times 27.2''$. The contour levels are -0.54, 0.54 ($2\sigma$), 1.08, and 1.62 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.2: The mosaic of the channel maps of NGC 4848. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.5'' \times 27.5''$. The contour levels are -0.56, 0.56 ($2\sigma$), and 1.12 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.3: The mosaic of the channel maps of CGCG 160-058. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.5'' \times 27.5''$. The contour levels are -0.56, 0.56 ($2\sigma$), 1.12, 1.68, and 2.24 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.4: The mosaic of the channel maps of KUG 1255+275, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.7'' \times 27.2''$. The contour levels are -0.54, 0.54 ($2\sigma$), 1.08, and 1.62 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.5: The mosaic of the channel maps of Mrk 057, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.7'' \times 27.2''$. The contour levels are -0.54, 0.54 ($2\sigma$), and 1.08 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.6: The mosaic of the channel maps of Mrk 058, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.3'' \times 27.6''$. The contour levels are -0.5, 0.5 ($2\sigma$), 1.0, and 1.5 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.7: The mosaic of the channel maps of CGCG 160-076, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $29.9'' \times 26.9''$. The contour levels are -0.54, 0.54 ($2\sigma$), 1.08, 2.16, 3.24, 4.32, 6.48, and 8.64 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.8: The mosaic of the channel maps of CGCG 160-086. The cross indicates the optical position. A noisy feature is seen in the south of the galaxy. The beam is indicated by the circle in the upper left panel, $35.2'' \times 33.0''$. The contour levels are -0.50, 0.50 ($2\sigma$), and 1.00 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.9: The mosaic of the channel maps of IC 4040. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $35.5'' \times 34.1''$. The contour levels are -0.26, 0.26 ($2\sigma$), 0.52, 0.78, and 1.04 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.10: The mosaic of the channel maps of IC 842. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $36.6'' \times 35.4''$. The contour levels are -0.44, 0.44 ($2\sigma$), 0.88, 1.76, and 2.64 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.11: The mosaic of the channel maps of KUG 1258+287, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.2'' \times 26.7''$. The contour levels are -0.56, 0.56 ($2\sigma$), 1.12, 1.68, and 2.24 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.12: The mosaic of the channel maps of NGC 4907. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $39.8'' \times 34.5''$. The contour levels are -0.44, 0.44 ($2\sigma$), and 0.88 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.13: The mosaic of the channel maps of NGC 4911. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $35.5'' \times 34.1''$. The contour levels are -0.26, 0.26 ($2\sigma$), 0.52, 0.78, and 1.04 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.14: The mosaic of the channel maps of FOCA 0195, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.2'' \times 26.7''$. The contour levels are -0.56, 0.56 ($2\sigma$), 1.12, 1.68, 2.24, and 2.80 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.15: The mosaic of the channel maps of NGC 4922. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $36.6'' \times 35.4''$. The contour levels are -2.2, -1.76, -1.32, -0.88, -0.44, 0.44 ($2\sigma$), and 0.88 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.16: The mosaic of the channel maps of CGCG 160-098, after Hanning smoothing. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $30.2'' \times 26.7''$. The contour levels are -0.56, 0.56 ($2\sigma$), 1.12, 1.68, and 2.24 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.17: The mosaic of the channel maps of NGC 4921. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $39.8'' \times 34.5''$. The contour levels are -0.46, 0.46 ($2\sigma$), 0.92, and 1.38 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.18: The mosaic of the channel maps of IC 4088. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $36.6'' \times 35.4''$. The contour levels are -0.46, 0.46 ($2\sigma$), 0.92, 1.84, 2.76, 4.60, 6.44, 8.28, 10.12, and 11.96 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.

Figure A.19: The mosaic of the channel maps of NGC 4926. The cross indicates the optical position, and the beam is indicated by the circle in the upper left panel, $35.2'' \times 33.0''$. The contour levels are -0.50, 0.50 ($2\sigma$), 1.00, and 1.50 mJy beam-1. Negative contours are dashed. Velocities are listed in each panel.