arXiv subjects

Brian R. McNamara

Publications and source records attributed to Brian R. McNamara.

59 records · Page 4Linked to original sources

arXiv2001

Chandra Observation of the Radio Source / X-ray Gas Interaction in the Cooling Flow Cluster Abell 2052

We present a Chandra observation of Abell 2052, a cooling flow cluster with a central cD that hosts the complex radio source 3C 317. The data reveal ``holes'' in the X-ray emission that are coincident with the radio lobes. The holes are surrounded by bright ``shells'' of X-ray emission. The data are consistent with the radio source displacing and compressing, and at the same time being confined by, the X-ray gas. The compression of the X-ray shells appears to have been relatively gentle and, at most, slightly transonic. The pressure in the X-ray gas (the shells and surrounding cooler gas) is approximately an order of magnitude higher than the minimum pressure derived for the radio source, suggesting that an additional source of pressure is needed to support the radio plasma. The compression of the X-ray shells has speeded up the cooling of the shells, and optical emission line filaments are found coincident with the brightest regions of the shells.

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arXiv2000

A Moderate Cluster Cooling Flow Model

We propose that the outer portions of cooling flows (CFs) in clusters of galaxies are frequently disrupted by radio jets, and that their effective ages are much shorter than the cluster ages. The inner regions, where the gas density is higher, are more difficult to disrupt, and may continue to harbor CFs even after disruption events. The main assumption of the proposed scenario is that, on a time scale of about 2-4 times 10^9 years the cD galaxies in CF clusters undergo powerful bursts of AGN activity that produce strong radio jets. The jets excite shock waves moving at several thousands km/sec and heat the CF region, hence terminating it in the outer regions. The total accreted mass due to the CF is an order of magnitude lower than the mass accreted according to the "standard" CF model (which assumes an undisturbed CF for a time equal to the age of the cluster). The scenario, therefore, brings to agreement the observations that a large fraction of clusters harbor CFs, that strong optical and radio activity are present only in the very inner regions of CFs, and the lack of a satisfactory reservoir of the expected (in the standard CF model) large mass that has been cooling over the life of the cluster.

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arXiv1998

An Alignment Effect in FR I Radio Galaxies: U-band Polarimetry of the Abell 2597 Cluster Central Galaxy

We have obtained U-band polarimetry of the spatially extended, blue optical continuum associated with the FR I radio source PKS 2322-122. PKS 2322-122 is located in the Abell 2597 cluster central galaxy. We find a three sigma upper limit to the degree of polarization of the optical continuum of less than 6%. This limit is inconsistent with the blue continuum being primarily scattered light or synchrotron radiation. We can therefore exclude models which attribute the blue continuum to scattered light from an active nucleus that is hidden from direct view. Essentially all of the data pertaining to the blue continuum along the radio source-the ``blue lobes''-indicate that they are regions of recent star formation that may have been induced by an interaction between the radio source and the cool ($<10^4$ K), surrounding gas. We compare the restframe U-band polarized luminosities and 1.4 GHz radio powers of A2597 and A1795 to those for several high redshift radio galaxies exhibiting the alignment effect. We suggest that the fundamental property distinguishing some powerful, high redshift radio galaxies exhibiting the alignment effect, and the lower-power, FR I radio galaxies in cooling flows that exhibit the blue lobe phenomenon, is the strength of the AGN.

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arXiv1996

Optical Properties of Cooling Flow Central Cluster Ellipticals

Central cluster galaxies in cooling flows show the signatures of gaseous accretion and ongoing star formation at rates ranging between 1-100 solar masses per year. Their blue morphologies usually reflect the low net angular momentum content of the less than 10,000 K gas from which the accretion population formed, and the effects of interactions between the cool gas and their FR I radio sources. For example, there is strong evidence that star formation is being triggered, in part, by interactions between the 10,000 K gas and the radio sources in some objects. Disk star formation on kiloparsec scales is rare in cooling flows. The optically determined star formation rates, assuming the Local initial mass function (IMF), are typically factors of 10-100 smaller than the cooling rates determined from X-ray observations, and signatures of the remaining material have not been identified outside of the X-ray band. The IMF is poorly understood in cooling flows; most of the cooling material may be deposited in low-mass stars or some other form of dark matter. Continued study of the interactions between radio sources and the intercluster medium will further our understanding of how elliptical galaxies, particularly radio ellipticals in the early universe, evolve.

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arXiv1996

ROSAT X-ray Observations of the Cooling Flow Cluster A2597

The cluster A2597 was observed in X-rays with the ROSAT PSPC and HRI detectors. The X-ray isophotes are oriented similarly to the optical isophotes of the central cD galaxy and to the isopleths of the galaxy distribution in the cluster, but are otherwise quite regular, suggesting that this cluster is reasonably relaxed and in hydrostatic equilibrium. The merged HRI and PSPC surface brightness profile is not adequately fit by a beta model because of the central X-ray surface brightness peak, indicating the presence of a cooling flow. If the central 108 arcsec in radius are excluded, an acceptable fit is found which gives beta = 0.64 but only an upper limit to the core radius, rcore < 78 arcsec. Within a radius of 2 Mpc, we found masses of Mgas = 1.2e14 Msun and Mtot = 6.5e14 Msun, and a gas mass fraction of about 19%. Both the overall cluster spectrum and the spatially resolved spectra within 300 kpc require the presence of both hot gas and a cooling flow in the spectrum. The spectrally determined total cooling rate of Mdot = 344 Msun/yr is in good agreement with those derived from analyses of the X-ray surface brightness profile from the Einstein IPC and the ROSAT HRI images. The ROSAT spatially resolved X-ray spectra indicate that the cooling component is distributed over the inner ~300 kpc in radius of the cluster. We do not detect any significant excess X-ray absorption toward the center of A2597, and we set a very conservative upper limit on the excess column in front of the cooling flow region of NH < 1.72e20 cm**-2.

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