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Active galactic nuclei play a crucial role in the accretion and ejection of gas in galaxies. Although their outflows are well studied, finding direct evidence of accretion has proved very difficult and has so far been done for very few sources. A promising way to study the significance of cold accretion is by observing the absorption of an active galactic nucleus's extremely bright radio emission by the cold gas lying along the line-of-sight. As such, we present ALMA CO(1-0) and CO(2-1) observations of the Hydra-A brightest cluster galaxy (z=0.054) which reveal the existence of cold, molecular gas clouds along the line-of-sight to the galaxy's extremely bright and compact mm-continuum source. They have apparent motions relative to the central supermassive black hole of between -43 and -4 km s$^{-1}$ and are most likely moving along stable, low ellipticity orbits. The identified clouds form part of a $\sim$$10^{9}$ $\text{M}_{\odot}$, approximately edge-on disc of cold molecular gas. With peak CO(2-1) optical depths of $\tau$=0.88 $^{+0.06}_{-0.06}$, they include the narrowest and by far the deepest absorption of this type which has been observed to date in a brightest cluster galaxy. By comparing the relative strengths of the lines for the most strongly absorbing region, we are able to estimate a gas temperature of $42^{+25}_{-11}$ K and line-of-sight column densities of $N_{CO}=2^{+3}_{-1}\times 10 ^{17} cm^{-2}$ and $N_{ H_{2} }=7^{+10}_{-4}\times 10 ^{20} cm^{-2}$., Comment: 11 pages, 8 figures, accepted to MNRAS

Active galactic nuclei play a crucial role in the accretion and ejection of gas in galaxies. Although their outflows are well studied, finding direct evidence of accretion has proved very difficult and has so far been done for very few sources. A promising way to study the significance of cold accretion is by observing the absorption of an active galactic nucleus's extremely bright radio emission by the cold gas lying along the line-of-sight. As such, we present ALMA CO(1-0) and CO(2-1) observations of the Hydra-A brightest cluster galaxy (z=0.054) which reveal the existence of cold, molecular gas clouds along the line-of-sight to the galaxy's extremely bright and compact mm-continuum source. They have apparent motions relative to the central supermassive black hole of between -43 and -4 km s$^{-1}$ and are most likely moving along stable, low ellipticity orbits. The identified clouds form part of a $\sim$$10^{9}$ $\text{M}_{\odot}$, approximately edge-on disc of cold molecular gas. With peak CO(2-1) optical depths of $\tau$=0.88 $^{+0.06}_{-0.06}$, they include the narrowest and by far the deepest absorption of this type which has been observed to date in a brightest cluster galaxy. By comparing the relative strengths of the lines for the most strongly absorbing region, we are able to estimate a gas temperature of $42^{+25}_{-11}$ K and line-of-sight column densities of $N_{CO}=2^{+3}_{-1}\times 10 ^{17} cm^{-2}$ and $N_{ H_{2} }=7^{+10}_{-4}\times 10 ^{20} cm^{-2}$., Comment: 11 pages, 8 figures, accepted to MNRAS

We illustrate the potential of using stellar velocity dispersion profiles of brightest cluster galaxies (BCGs), in combination with X-ray and weak-lensing derived cluster mass profiles, to constrain the matter distribution from the very centre (1 kpc) to the outskirts (1000 kpc) of galaxy clusters. We have obtained long-slit spectroscopy of a small number of BCGs in CLASH (Cluster Lensing and Supernova Survey with Hubble) clusters at the Southern African Large Telescope (SALT) with the primary goal of measuring their stellar kinematics. The new data extends the observed total mass profile of the cluster over another order of magnitude in radius, which places a much stronger constraint on the dark matter distribution, thereby leveraging the enormous investment in mass-profile measurements at larger radii in these clusters. Here, we discuss the observations and apply the methodology to one of the clusters, RXJ2129.7+0005 (z 0:23), to find results consistent with a mass profile slope that becomes shallower than the typical Navarro-Frenk-White (NFW) profile when dynamical data in the very innermost region of the cluster is also included in its mass profile

We illustrate the potential of using stellar velocity dispersion profiles of brightest cluster galaxies (BCGs), in combination with X-ray and weak-lensing derived cluster mass profiles, to constrain the matter distribution from the very centre (1 kpc) to the outskirts (1000 kpc) of galaxy clusters. We have obtained long-slit spectroscopy of a small number of BCGs in CLASH (Cluster Lensing and Supernova Survey with Hubble) clusters at the Southern African Large Telescope (SALT) with the primary goal of measuring their stellar kinematics. The new data extends the observed total mass profile of the cluster over another order of magnitude in radius, which places a much stronger constraint on the dark matter distribution, thereby leveraging the enormous investment in mass-profile measurements at larger radii in these clusters. Here, we discuss the observations and apply the methodology to one of the clusters, RXJ2129.7+0005 (z 0:23), to find results consistent with a mass profile slope that becomes shallower than the typical Navarro-Frenk-White (NFW) profile when dynamical data in the very innermost region of the cluster is also included in its mass profile

We illustrate the potential of using stellar velocity dispersion profiles of brightest cluster galaxies (BCGs), in combination with X-ray and weak-lensing derived cluster mass profiles, to constrain the matter distribution from the very centre (1 kpc) to the outskirts (1000 kpc) of galaxy clusters. We have obtained long-slit spectroscopy of a small number of BCGs in CLASH (Cluster Lensing and Supernova Survey with Hubble) clusters at the Southern African Large Telescope (SALT) with the primary goal of measuring their stellar kinematics. The new data extends the observed total mass profile of the cluster over another order of magnitude in radius, which places a much stronger constraint on the dark matter distribution, thereby leveraging the enormous investment in mass-profile measurements at larger radii in these clusters. Here, we discuss the observations and apply the methodology to one of the clusters, RXJ2129.7+0005 (z 0:23), to find results consistent with a mass profile slope that becomes shallower than the typical Navarro-Frenk-White (NFW) profile when dynamical data in the very innermost region of the cluster is also included in its mass profile

We illustrate the potential of using stellar velocity dispersion profiles of brightest cluster galaxies (BCGs), in combination with X-ray and weak-lensing derived cluster mass profiles, to constrain the matter distribution from the very centre (1 kpc) to the outskirts (1000 kpc) of galaxy clusters. We have obtained long-slit spectroscopy of a small number of BCGs in CLASH (Cluster Lensing and Supernova Survey with Hubble) clusters at the Southern African Large Telescope (SALT) with the primary goal of measuring their stellar kinematics. The new data extends the observed total mass profile of the cluster over another order of magnitude in radius, which places a much stronger constraint on the dark matter distribution, thereby leveraging the enormous investment in mass-profile measurements at larger radii in these clusters. Here, we discuss the observations and apply the methodology to one of the clusters, RXJ2129.7+0005 (z 0:23), to find results consistent with a mass profile slope that becomes shallower than the typical Navarro-Frenk-White (NFW) profile when dynamical data in the very innermost region of the cluster is also included in its mass profile

The physical relationship between low-excitation gas filaments at ~10^4 K, seen in optical line emission, and diffuse X-ray emitting coronal gas at ~10^7 K in the centers of many galaxy clusters is not understood. It is unclear whether the ~10^4 K filaments have cooled and condensed from the ambient hot (~10^7 K) medium or have some other origin such as the infall of cold gas in a merger, or the disturbance of an internal cool reservoir of gas by nuclear activity. Observations of gas at intermediate temperatures (~10^5-10^6 K) can potentially reveal whether the central massive galaxies are gaining cool gas through condensation or losing it through conductive evaporation and hence identify plausible scenarios for transport processes in galaxy cluster gas. Here we present spectroscopic detection of ~10^5 K gas spatially associated with the H-alpha filaments in a central cluster galaxy, M87 in the Virgo Cluster. The measured emission-line fluxes from triply ionized carbon (CIV 1549 A) and singly ionized helium (HeII 1640 A) are consistent with a model in which thermal conduction determines the interaction between hot and cold phases., Comment: 10 pages, 2 figures; to appear in ApJL

The physical relationship between low-excitation gas filaments at ~10^4 K, seen in optical line emission, and diffuse X-ray emitting coronal gas at ~10^7 K in the centers of many galaxy clusters is not understood. It is unclear whether the ~10^4 K filaments have cooled and condensed from the ambient hot (~10^7 K) medium or have some other origin such as the infall of cold gas in a merger, or the disturbance of an internal cool reservoir of gas by nuclear activity. Observations of gas at intermediate temperatures (~10^5-10^6 K) can potentially reveal whether the central massive galaxies are gaining cool gas through condensation or losing it through conductive evaporation and hence identify plausible scenarios for transport processes in galaxy cluster gas. Here we present spectroscopic detection of ~10^5 K gas spatially associated with the H-alpha filaments in a central cluster galaxy, M87 in the Virgo Cluster. The measured emission-line fluxes from triply ionized carbon (CIV 1549 A) and singly ionized helium (HeII 1640 A) are consistent with a model in which thermal conduction determines the interaction between hot and cold phases., Comment: 10 pages, 2 figures; to appear in ApJL

Gas at intermediate temperature between the hot X-ray emitting coronal gas in galaxies at the centers of galaxy clusters, and the much cooler optical line emitting filaments, yields information on transport processes and plausible scenarios for the relationship between X-ray cool cores and other galactic phenomena such as mergers or the onset of an active galactic nucleus. Hitherto, detection of intermediate temperature gas has proven elusive. Here, we present FUV imaging of the "low excitation" emission filaments of M87 and show strong evidence for the presence of CIV 1549 A emission which arises in gas at temperature ~10^5K co-located with Halpha+[NII] emission from cooler ~10^4K gas. We infer that the hot and cool phases are in thermal communication, and show that quantitatively the emission strength is consistent with thermal conduction, which in turn may account for many of the observed characteristics of cool core galaxy clusters., Comment: Accepted for publication in ApJ Letters

We are learning much about how structure forms, in particular how clusters as nodes in the cosmic web evolve and accrete matter, and about the physical processes within these objects. In the next decade, the study of clusters will enable us to tackle important questions regarding the nature of Dark Matter and Dark Energy, how clusters co-evolve with super-massive black holes at their centers, and to advance our knowledge about fundamental plasma astrophysics. This science white paper outlines the key questions and research opportunities in cluster astrophysics that are emerging in the coming decade and beyond, and serves as an overview to other cluster related white papers., Comment: 8 pages, 4 figures. Science White Paper submitted to CFP and GCT panels of Astro2010

Gas at intermediate temperature between the hot X-ray emitting coronal gas in galaxies at the centers of galaxy clusters, and the much cooler optical line emitting filaments, yields information on transport processes and plausible scenarios for the relationship between X-ray cool cores and other galactic phenomena such as mergers or the onset of an active galactic nucleus. Hitherto, detection of intermediate temperature gas has proven elusive. Here, we present FUV imaging of the "low excitation" emission filaments of M87 and show strong evidence for the presence of CIV 1549 A emission which arises in gas at temperature ~10^5K co-located with Halpha+[NII] emission from cooler ~10^4K gas. We infer that the hot and cool phases are in thermal communication, and show that quantitatively the emission strength is consistent with thermal conduction, which in turn may account for many of the observed characteristics of cool core galaxy clusters., Comment: Accepted for publication in ApJ Letters

We are learning much about how structure forms, in particular how clusters as nodes in the cosmic web evolve and accrete matter, and about the physical processes within these objects. In the next decade, the study of clusters will enable us to tackle important questions regarding the nature of Dark Matter and Dark Energy, how clusters co-evolve with super-massive black holes at their centers, and to advance our knowledge about fundamental plasma astrophysics. This science white paper outlines the key questions and research opportunities in cluster astrophysics that are emerging in the coming decade and beyond, and serves as an overview to other cluster related white papers., Comment: 8 pages, 4 figures. Science White Paper submitted to CFP and GCT panels of Astro2010

We describe our ongoing program designed to measure the SN-Ia rate in a sample of massive z=0.5-0.9 galaxy clusters. The SN-Ia rate is a poorly known observable, especially at high z, and in cluster environments. The SN rate and its redshift dependence can serve as powerful discrimiminants for a number of key issues in astrophysics and cosmology. Our observations will put clear constraints on the characteristic SN-Ia ``delay time'', the typical time between the formation of a stellar population and the explosion of some of its members as SNe-Ia. Such constraints can exclude entire categories of SN-Ia progenitor models, since different models predict different delays. These data will also help to resolve the question of the dominant source of the high metallicity in the intracluster medium (ICM) - SNe-Ia, or core-collapse SNe from an early stellar population with a top-heavy IMF, perhaps those population III stars responsible for the early re-ionization of the Universe. Since clusters are excellent laboratories for studying enrichment (they generally have a simple star-formation history, and matter cannot leave their deep potentials), the results will be relevant for understanding metal enrichment in general, and the possible role of first generation stars in early Universal enrichment. Observations obtained so far during cycles 14 and 15 yield many SNe in our cluster fields, but our follow-up campaign reveals most are not in cluster galaxies., Comment: To appear in the proceedings of the meeting "The Multicoloured Landscape of Compact Objects and their Explosive Origins", Cefalu, Italy, June 2006, to be published by AIP, Eds. L. Burderi et al

We present a systematic investigation of X-ray thermal coronae in 157 early-type galaxies and 22 late-type galaxies from a survey of 25 hot (kT>3 keV), nearby (z<0.05) clusters, based on CHANDRA archival data. Cool galactic coronae (kT=0.5-1.1 keV generally) have been found to be very common, >60% in NIR selected galaxies that are more luminous than 2L*, and >40% in L* < L_Ks < 2L* galaxies. These embedded coronae in hot clusters are generally smaller (1.5-4 kpc radii), less luminous (<~ 10^41 erg s^-1), and less massive (10^6.5-10^8 M_solar}) than coronae in poor environments, demonstrating the negative effects of hot cluster environments on galactic coronae. Nevertheless, these coronae still manage to survive ICM stripping, evaporation, rapid cooling, and powerful AGN outflows, making them a rich source of information about gas stripping, microscopic transport, and feedback processes in the cluster environment. Heat conduction across the boundary of the coronae has to be suppressed by a factor of >100, which implies the X-ray gas in early-type galaxies is magnetized and the magnetic field plays an important role in energy transfer. Stripping through transport processes (viscosity or turbulence) also needs to be suppressed by at least a factor of ten at the coronal boundary... (abridged) Diffuse thermal coronae have also been detected in at least 8 of 22 late-type (Sb or later) galaxies in our sample. Evidence for enhanced star formation triggered by the ICM pressure has been found in four late-type galaxies. The fraction of luminous X-ray AGN (>10^41 ergs s^-1) is not small (~ 5%) in our sample., Comment: 40 pages, 3 tables, 28 figures (9 in color), emulateapj5.sty, accepted by ApJ, revised in many places but conclusions unchanged (add X-ray AGN fraction), the full-resolution and complete version at http://www.pa.msu.edu/~sunm/coronae_all_v1.5_emuapj.ps.gz

We describe our ongoing program designed to measure the SN-Ia rate in a sample of massive z=0.5-0.9 galaxy clusters. The SN-Ia rate is a poorly known observable, especially at high z, and in cluster environments. The SN rate and its redshift dependence can serve as powerful discrimiminants for a number of key issues in astrophysics and cosmology. Our observations will put clear constraints on the characteristic SN-Ia ``delay time'', the typical time between the formation of a stellar population and the explosion of some of its members as SNe-Ia. Such constraints can exclude entire categories of SN-Ia progenitor models, since different models predict different delays. These data will also help to resolve the question of the dominant source of the high metallicity in the intracluster medium (ICM) - SNe-Ia, or core-collapse SNe from an early stellar population with a top-heavy IMF, perhaps those population III stars responsible for the early re-ionization of the Universe. Since clusters are excellent laboratories for studying enrichment (they generally have a simple star-formation history, and matter cannot leave their deep potentials), the results will be relevant for understanding metal enrichment in general, and the possible role of first generation stars in early Universal enrichment. Observations obtained so far during cycles 14 and 15 yield many SNe in our cluster fields, but our follow-up campaign reveals most are not in cluster galaxies., Comment: To appear in the proceedings of the meeting "The Multicoloured Landscape of Compact Objects and their Explosive Origins", Cefalu, Italy, June 2006, to be published by AIP, Eds. L. Burderi et al

We present a systematic investigation of X-ray thermal coronae in 157 early-type galaxies and 22 late-type galaxies from a survey of 25 hot (kT>3 keV), nearby (z<0.05) clusters, based on CHANDRA archival data. Cool galactic coronae (kT=0.5-1.1 keV generally) have been found to be very common, >60% in NIR selected galaxies that are more luminous than 2L*, and >40% in L* < L_Ks < 2L* galaxies. These embedded coronae in hot clusters are generally smaller (1.5-4 kpc radii), less luminous (<~ 10^41 erg s^-1), and less massive (10^6.5-10^8 M_solar}) than coronae in poor environments, demonstrating the negative effects of hot cluster environments on galactic coronae. Nevertheless, these coronae still manage to survive ICM stripping, evaporation, rapid cooling, and powerful AGN outflows, making them a rich source of information about gas stripping, microscopic transport, and feedback processes in the cluster environment. Heat conduction across the boundary of the coronae has to be suppressed by a factor of >100, which implies the X-ray gas in early-type galaxies is magnetized and the magnetic field plays an important role in energy transfer. Stripping through transport processes (viscosity or turbulence) also needs to be suppressed by at least a factor of ten at the coronal boundary... (abridged) Diffuse thermal coronae have also been detected in at least 8 of 22 late-type (Sb or later) galaxies in our sample. Evidence for enhanced star formation triggered by the ICM pressure has been found in four late-type galaxies. The fraction of luminous X-ray AGN (>10^41 ergs s^-1) is not small (~ 5%) in our sample., Comment: 40 pages, 3 tables, 28 figures (9 in color), emulateapj5.sty, accepted by ApJ, revised in many places but conclusions unchanged (add X-ray AGN fraction), the full-resolution and complete version at http://www.pa.msu.edu/~sunm/coronae_all_v1.5_emuapj.ps.gz

We present the discovery of a 70 kpc X-ray tail behind the small late-type galaxy ESO137-001 in the nearby, hot (T=6.5 keV) merging cluster A3627, from both Chandra and XMM observations. The tail has a length-to-width ratio of ~ 10. It is luminous (L_{0.5-2 keV} ~ 10^41 ergs s^-1, with a temperature of ~ 0.7 keV and an X-ray M_gas of ~ 10^9 M_solar (~ 10% of the galaxy's stellar mass). We interpret this tail as the stripped interstellar medium of ESO137-001 mixed with the hot cluster medium, when this blue galaxy is being converted into a gas-poor galaxy. Three X-ray point sources are detected in the axis of the tail, which may imply active star formation in the tail. The straightness and narrowness of the tail also implies that the ICM turbulence is not strong on scales of 20 - 70 kpc., Comment: 5 pages, 1 color figure, minor revision, accepted by ApJL (Version with the full-resolution figure available at http://www.pa.msu.edu/~sunm/eso137_001_v1.1.ps.gz)

The amount and nature of dark energy (DE) can be tightly constrained by measuring the spatial correlation features and evolution of a sample of ~ 100,000 galaxy clusters over the redshift range 0

The amount and nature of dark energy (DE) can be tightly constrained by measuring the spatial correlation features and evolution of a sample of ~ 100,000 galaxy clusters over the redshift range 0

We present the discovery of a 70 kpc X-ray tail behind the small late-type galaxy ESO137-001 in the nearby, hot (T=6.5 keV) merging cluster A3627, from both Chandra and XMM observations. The tail has a length-to-width ratio of ~ 10. It is luminous (L_{0.5-2 keV} ~ 10^41 ergs s^-1, with a temperature of ~ 0.7 keV and an X-ray M_gas of ~ 10^9 M_solar (~ 10% of the galaxy's stellar mass). We interpret this tail as the stripped interstellar medium of ESO137-001 mixed with the hot cluster medium, when this blue galaxy is being converted into a gas-poor galaxy. Three X-ray point sources are detected in the axis of the tail, which may imply active star formation in the tail. The straightness and narrowness of the tail also implies that the ICM turbulence is not strong on scales of 20 - 70 kpc., Comment: 5 pages, 1 color figure, minor revision, accepted by ApJL (Version with the full-resolution figure available at http://www.pa.msu.edu/~sunm/eso137_001_v1.1.ps.gz)

A Chandra image of the central 100 kpc of the Abell 2597 cluster of galaxies shows bright, irregular, X-ray emission within the central dominant cluster galaxy (CDG), and two low surface brightness cavities located 30 kpc from the CDG's nucleus. Unlike the cavities commonly seen in other clusters, Abell 2597's ``ghost'' cavities are not coincident with the bright central radio source. Instead, they appear to be associated with faint, extended radio emission seen in a deep VLA radio map. We interpret the ghost cavities as buoyantly-rising relics of a radio outburst that occurred between 50--100 Myr ago. The demography of cavities in the few clusters studied thus far shows that galactic radio sources experience recurrent outbursts on a $\sim 100$ Myr timescale. Over the lifetime of a cluster, ghost cavities emerging from CDGs deposit $\gae 10^{59-61}$ erg of energy into the intracluster medium. If a significant fraction of this energy is deposited as magnetic field, it would account for the high field strengths in the cooling flow regions of clusters. The similarity between the central cooling time of the keV gas and the radio cycling timescale suggests that feedback between cooling gas and the radio source may be retarding or quenching the cooling flow., Comment: includes two color and two black and white figures. Accepted for publication in the Astrophysical Journal

A Chandra image of the central 100 kpc of the Abell 2597 cluster of galaxies shows bright, irregular, X-ray emission within the central dominant cluster galaxy (CDG), and two low surface brightness cavities located 30 kpc from the CDG's nucleus. Unlike the cavities commonly seen in other clusters, Abell 2597's ``ghost'' cavities are not coincident with the bright central radio source. Instead, they appear to be associated with faint, extended radio emission seen in a deep VLA radio map. We interpret the ghost cavities as buoyantly-rising relics of a radio outburst that occurred between 50--100 Myr ago. The demography of cavities in the few clusters studied thus far shows that galactic radio sources experience recurrent outbursts on a $\sim 100$ Myr timescale. Over the lifetime of a cluster, ghost cavities emerging from CDGs deposit $\gae 10^{59-61}$ erg of energy into the intracluster medium. If a significant fraction of this energy is deposited as magnetic field, it would account for the high field strengths in the cooling flow regions of clusters. The similarity between the central cooling time of the keV gas and the radio cycling timescale suggests that feedback between cooling gas and the radio source may be retarding or quenching the cooling flow., Comment: includes two color and two black and white figures. Accepted for publication in the Astrophysical Journal

A Chandra image of the central 100 kpc of the Abell 2597 cluster of galaxies shows bright irregular X-ray emission within the central dominant cluster galaxy (CDG) and two low surface brightness cavities located 30 kpc from the nucleus of the CDG. Unlike the cavities commonly seen in other clusters, the "ghost" cavities in Abell 2597 are not coincident with the bright central radio source. Instead, they appear to be associated with faint extended radio emission seen in a deep Very Large Array radio map. We interpret the ghost cavities as buoyantly rising relics of a radio outburst that occurred between 50 and 100 Myr ago. The demography of cavities in the few clusters studied thus far shows that galactic radio sources experience recurrent outbursts on an ∼100 Myr timescale. Over the lifetime of a cluster, ghost cavities emerging from CDGs deposit &gsim;1059–1061 ergs of energy into the intracluster medium. If a significant fraction of this energy is deposited as magnetic field, it would account for the high field strengths in the cooling flow regions of clusters. The similarity between the central cooling time of the keV gas and the radio cycling timescale suggests that feedback between cooling gas and the radio source may be retarding or quenching the cooling flow.

A Chandra image of the central 100 kpc of the Abell 2597 cluster of galaxies shows bright irregular X-ray emission within the central dominant cluster galaxy (CDG) and two low surface brightness cavities located 30 kpc from the nucleus of the CDG. Unlike the cavities commonly seen in other clusters, the "ghost" cavities in Abell 2597 are not coincident with the bright central radio source. Instead, they appear to be associated with faint extended radio emission seen in a deep Very Large Array radio map. We interpret the ghost cavities as buoyantly rising relics of a radio outburst that occurred between 50 and 100 Myr ago. The demography of cavities in the few clusters studied thus far shows that galactic radio sources experience recurrent outbursts on an ∼100 Myr timescale. Over the lifetime of a cluster, ghost cavities emerging from CDGs deposit &gsim;1059–1061 ergs of energy into the intracluster medium. If a significant fraction of this energy is deposited as magnetic field, it would account for the high field strengths in the cooling flow regions of clusters. The similarity between the central cooling time of the keV gas and the radio cycling timescale suggests that feedback between cooling gas and the radio source may be retarding or quenching the cooling flow.

A Chandra image of the central 100 kpc of the Abell 2597 cluster of galaxies shows bright irregular X-ray emission within the central dominant cluster galaxy (CDG) and two low surface brightness cavities located 30 kpc from the nucleus of the CDG. Unlike the cavities commonly seen in other clusters, the "ghost" cavities in Abell 2597 are not coincident with the bright central radio source. Instead, they appear to be associated with faint extended radio emission seen in a deep Very Large Array radio map. We interpret the ghost cavities as buoyantly rising relics of a radio outburst that occurred between 50 and 100 Myr ago. The demography of cavities in the few clusters studied thus far shows that galactic radio sources experience recurrent outbursts on an ∼100 Myr timescale. Over the lifetime of a cluster, ghost cavities emerging from CDGs deposit &gsim;1059–1061 ergs of energy into the intracluster medium. If a significant fraction of this energy is deposited as magnetic field, it would account for the high field strengths in the cooling flow regions of clusters. The similarity between the central cooling time of the keV gas and the radio cycling timescale suggests that feedback between cooling gas and the radio source may be retarding or quenching the cooling flow.

A Chandra image of the central 100 kpc of the Abell 2597 cluster of galaxies shows bright irregular X-ray emission within the central dominant cluster galaxy (CDG) and two low surface brightness cavities located 30 kpc from the nucleus of the CDG. Unlike the cavities commonly seen in other clusters, the "ghost" cavities in Abell 2597 are not coincident with the bright central radio source. Instead, they appear to be associated with faint extended radio emission seen in a deep Very Large Array radio map. We interpret the ghost cavities as buoyantly rising relics of a radio outburst that occurred between 50 and 100 Myr ago. The demography of cavities in the few clusters studied thus far shows that galactic radio sources experience recurrent outbursts on an ∼100 Myr timescale. Over the lifetime of a cluster, ghost cavities emerging from CDGs deposit &gsim;1059–1061 ergs of energy into the intracluster medium. If a significant fraction of this energy is deposited as magnetic field, it would account for the high field strengths in the cooling flow regions of clusters. The similarity between the central cooling time of the keV gas and the radio cycling timescale suggests that feedback between cooling gas and the radio source may be retarding or quenching the cooling flow.

We present a deep ASCA observation of a Broad Absorption Line Quasar (BALQSO) PG0946+301. The source was clearly detected in one of the gas imaging spectrometers, but not in any other detector. If BALQSOs have intrinsic X-ray spectra similar to normal radio-quiet quasars, our observations imply that there is Thomson thick X-ray absorption (N_H >~10^{24} cm^{-2}) toward PG0946+301. This is the largest column density estimated so far toward a BALQSO. The absorber must be at least partially ionized and may be responsible for attenuation in the optical and UV. If the Thomson optical depth toward BALQSOs is close to one, as inferred here, then spectroscopy in hard X-rays with large telescopes like XMM would be feasible., Comment: 6 pages, LaTex, submitted to ApJL

We present a deep ASCA observation of a broad absorption line quasar (BALQSO) PG 0946+301. The source was clearly detected in one of the gas imaging spectrometers, but not in any other detector. If BALQSOs have intrinsic X-ray spectra similar to normal radio-quiet quasars, our observations imply that there is Thomson thick X-ray absorption (NH ≳ 1024 cm-2) toward PG 0946+301. This is the largest column density estimated so far toward a BALQSO. The absorber must be at least partially ionized and may be responsible for attenuation in the optical and UV. If the Thomson optical depth toward BALQSOs is close to 1, as inferred here, then spectroscopy in hard X-rays with large telescopes like XMM would be feasible.

We present a deep ASCA observation of a Broad Absorption Line Quasar (BALQSO) PG0946+301. The source was clearly detected in one of the gas imaging spectrometers, but not in any other detector. If BALQSOs have intrinsic X-ray spectra similar to normal radio-quiet quasars, our observations imply that there is Thomson thick X-ray absorption (N_H >~10^{24} cm^{-2}) toward PG0946+301. This is the largest column density estimated so far toward a BALQSO. The absorber must be at least partially ionized and may be responsible for attenuation in the optical and UV. If the Thomson optical depth toward BALQSOs is close to one, as inferred here, then spectroscopy in hard X-rays with large telescopes like XMM would be feasible., Comment: 6 pages, LaTex, submitted to ApJL