/4/77=_-?f_7 1I¢ -ci.2i Investigation Relative to the -L= Roentgen Satellite (ROSAT) %P NASA Grant NAG5-1536 -__:._.._.._:._._........ Semiannual _port Nos. 4 and 5 Period 15 October:]_92 through 15 October 1993 o" N 0 Principa] Investigators I w,,, r,,- (See At-tached) 4" U 0 o, t- N Z :_ 0 O- cO January 1994 _b Prepared for: Aeronautics and Space Administration ;pace Flight Center Ireenbelt, Maryland 20771 -Smitl_soni_-n' institution Astropl_ys aT-Observat ory Cambridge, Massachusetts 02138 _?he Smithsonian Astrophysical Observatory I-ll is a member of the _arvard-Smithsonian Center for Astrophysics 2:::27-:27:--- cer for this grant isDr. Robert Petre, Code 666, Sciences Directorate, Goddard Space Flight C( ............................ -'7--.................... 1 Investigation Relative to ROSAT 1.1 PR 666-27127 (P.I.: Martin S. Elvis) Papers were written describing several major results as a result of this program. Others are in preparation. P2095-5-89RI -- What Does a Normal Quasar Look Like in X-rays? . Objects observed in this program have been combined with those in a study by A. Laor et al. to increase the sample size and will be reported there. A paper is in preparation on the combined sample. P2094-5-89RI -- complexity in Quasar X-ray Spectra: XUV Excesses o This work proceeds well and a paper is in preparation indicating a high energy excess. This program has been critically dependent on the energy calibration of the PSPC, and indeed our investigations have assisted significantly in understanding that calibration through our discussions with GSFC and MPE. P2121-5-89RI -- Structure of Seyfert Galaxies with Known X-ray Extent o Paper on NGC1068 published in Ap.J. 1992. Demonstrated that ,._50% of the soft x- ray emission in NGC1068 is extended on a galaxy sized scale, and is not nuclear. The HRI hardness ratio shows the extended emission is stronger at 1 keV than at 0.25 keV, suggesting that the emission from Fe-L lines seen in BBXRT is extended and thermal. Our A01 observation of NGC 4151 was not scheduled until A04 (May 93) and the data has not been receive yet. ° P2079-5-89RI -- Quasar Spectra Beyond the Redshift "Cut-Off" One paper has been published in Ap.J.(Letters) 1992, another is in press with Ap.J. They describe the results on six high redshift quasars, including the discovery of unex- pected absorption toward these objects. The implications of these results are discussed in detail. A third paper describing the multiwavelength properties of these quasars from x-ray to radio is in preparation. Refereed Papers An X-ray Image of the Seyfert Galaxy NGC1068 (A.S. Wilson, M. Elvis, A. Lawrence, and J. Bland-Hawthorn), Ap.J.(Letters), 391, L75. PKS0438-436: A High Redshift Quasar with Strong X-ray Absorption (B.J. Wilkes, M. Elvis, H. Tananbaum, J.C. McDowell, and A. Lawrence), Ap.J. (Letters), 393, L1. Absorption in X-ray Spectra of High Redshift Quasars (M. Elvis, F. Fiore, B.J. Wilkes, J.C. McDowell, and J. Bechtold, Ap.J. 422, in press (Feb. 10). 1.2 PR 666-27036 (P.I.: Francis A. Primini) P2092-5-89RI-- High ResolutionObservationsof the CentralRegionof M31 A comprehensivestudy of the X-ray source population in the central bulge of M31 ap- peared in Vol. 410 of the Astrophysical Journal (June 20, 1993). This study includes X-ray source identifications, luminosity measurements, luminosity functions for all the total source population and for X-ray globular clusters, estimates for individual source variability, and a preliminary measurement of the unresolved X-ray emission with 1 kpc of the nucleus of M31. 1.3 PR 666-27513 (P.I.: Giuseppina Fabbiano) P2096-5-89RI -- The X-ray Emission of Low-X-ray-Luminosity Early-Type Galaxies: Gas Versus Compact Sources Two papers submitted to Ap.J.: The first reporting the results of the ROSAT observa- tions of NGC4365 and NGC4382, the second discussing these results in the context of an evolutionary model for the ISM. Copies of these papers are included in Appendix A. 1.4 PR 666-27512 (P.I.: Daniel E. Harris) P2098-5-89RI -- Interaction Between Cluster GAs and Radio Features of Cygnus A Although this was a ROSAT AO-1 project, the data were not delivered until Nov 1992. Preliminary evaluation of the image demonstrated: (a) the "6-month aspect offset syndrome" is present in the data, with an amplitude of approximately 15"; (b) there is discreet emission from the regions of the radio hot-spots; and (c) there appears to be a diminution of emission coincident with the radio lobes. C. Carilli, CoI from NRAO visited the CfA for a week to work on data reduction (Feb, 93). We performed 3 operations to improve the spatial characteristics of the image. First we examined the PHA distribution of the main cluster gas, the features in the radio hotspot region, and the background. We found that if we cut channels 8-15, we would loose 3% of the source counts, but 21registration we performed two independent shifts. In the first, we used a smoothed version of each of the 29 obis to measure the peak of the main cluster emission, and then shifted each obi and coadded. In the second method, we divided the data into 5 time segments: 91apr, 91nov, 91dec, 92apr, and 92may. The position of a weak unresolved source 41off axis was then used to calculate the required shifts. Analysis of the hotspot emission showed that the East spot is resolved with gross structure similar to the radio morphology. Counts were measured with "gun-sight" binning. Following conversion to flux with Obstime software, we used the observed radio spectrum to predict the synchrotron self Compton (SSC) contribution to the x-ray emission and found agreement with the measurements. We have been in contact with Biermann and Mannheim (Germany) to discuss the relevance of their model for emission from "proton induced cascades". This is a 'sister' process to the SSC emission. Perley, another Co-I from the NRAO visited for a weekin April '93, and pursuedGould's and Marscher'spublished methodsfor dealing with SSCemission.Harris hasobtainedcodewhichusesnumericalmethodsfor calculating SSCspectra,andthis will be usedto checkour analytic estimates.Wealsoestimatedthe parameterstoexplainthehotspotemissionasanextensionofthe radiosynchrotronspectrum or asthermal emission.Both ofthesepossibilitiesappearunlikely. Thermalemissionfrom the bowshockhasbeenevaluated,andwearealsoinvestigating explanationsfor the decreasein emissioncoincidentwith theinner parts of theradio lobes. Perleyand Harris met with D. Clarketo discussa collaborationon numericalsimulations to modelthe jet evolutionandlobestructureto seeif wecanreproducesomeofthe details of the interaction betweenthe gasand radio features. Wehaveperformeda King model subtract, which emphasizesthe effectof the "cavity" in the to gas,aswell asaccentuating the hot spot emissionand the coresourcewhich is apparentlyunresolvedand coincident with the optical galaxy. Weplan afirst paperwhichwill concentrateonthe hotspotemission.Subsequentpapers will dealwith the lobe/gasinteractionandother aspectsofthe data. Resultsarealsobeing reported at a varietyof talks by the investigators. 1.5 PR 666-27514 (P.I.: Christine Jones-Forman) P2124-5-89RI -- Hot Gas and Dark Halos in Early-Type Galaxies We are now completing a paper for submission to the Astrophysical Journal in which we report the results of our analysis of a deep 29 ksec ROSAT PSPC observation of the Fornax cluster which was centered on NGC1399. We use the observed x-ray surface brightness profile and gas temperature profile to determine the distribution of gravitating mass. The x-ray parameters required for measuring the gravitational mass can be traced to a distance of 18/arcmin from NGC1399, a distance of 126 kpc, assuming a distance modulus of 31.9 (equivalent to 24.0 Mpc; Ferguson 1989). We derive and discuss the radial distributions of the mass components of the system-the gas mass, the stellar mass in galaxies, and the dynamical mass. For the gaseous corona around NGC1399, we also measured the iron abundance to be approximately solar and constant with radius. P2099-5-89RI -- A Gravitational Lens in X-rays - 0957+461 The gravitational lens 0957+561 is comprised of a quasar at a redshift of 1.41 that is lensed by an intervening galaxy and surrounding cluster at a redshift of 0.36. A paper "ROSAT Images of the Gravitationally Lensed Quasar 0957+561" by Chartas, Falco, For- man, Jones, Schild and Shapiro was presented at the 31st Liege International Astrophysical Colloquium "Gravitational Lenses in the Universe" and will be submitted to the conference proceedings. From our analysis of the ROSAT observations, we find that the x-ray flux ratio of th two quasar images is significantly greater than the optical flux ratio. Our observations suggest that one of the quasar images may be microlensed by stars in the lensing galaxy. From analysis of a ROSAT PSPC observation, obtained from the archive, we find that the energy spectra of the quasar images is extremely soft. 3 1.6 PR 666-27511 (P.I.: Ginevra Trinchieri) P2102-5-89RI -- How Massive are Early-Type Galaxies? The spatial analysis of PSPC data of NGC4636, a bright early type galaxy at the outskirts of the Virgo Cluster, indicates that the source is extended, with a smoothly decreasing radial profile out to r/sim6' - -8', after which radius the profiles flattens significantly and an be detected out to r/siml8', or roughly the round support structure of the PSPC. A thin thermal spectrum with low energy absorption is used to fit the spectral count distribution. Several concentric annuli are analyzed separately, to obtain information on the spectral parameters in different regions. We cannot fit a single temperature model to the data, if we assume a gas with 100% cosmic abundances: multitemperature fits are required in the innermost 2'. This requirement is relaxed for low (20%) cosmic abundances. A temperature gradient is observed in the inner 4' - 6', for kT increasing outwards from ,--0.5 to ,_1 keV. A paper containing the details of the analysis and the results in upon completion. Pre- liminary results have been presented at the ROSAT Data Analysis and Science workshop held in November 1992 in Boston, and at the Kiel meeting in Germany (Mary 8-12, 1993). 1.7 PR 666-27229 (P.I.: Leon Golub) P2106-5-89RI -- Coronal Physics of the Lower Main Sequence: Relationships Among X-rays, Radio Emission and Magnetic Fields No new input was given for this report. 1.8 PR 666-27509 (P.I.: Jay Bookbinder) P2108-5-89RI -- X-ray Observations of the Eclipsing Millisecond Pulsar No new input was given for this report. 1.9 PR 666-27126 (P.I.: Frederick D. Seward) P2114-5-89RI -- Three Crab-Like SNR in the Large Magellanic Cloud One HRI observation was approved from this proposal. The exposure was made in July 1990. The purpose was to detect the outer shell of a SNR in the LMC. The observation is difficult because the remnant has an x-ray bright interior where an energetic 50 millisecond pulsar resides. The observation was success. The shell was observed and delineated. 23% of the x-rays originate in the shell. Measured properties of the shell ware used to derive the energy release of the supernova explosion. A paper describing these results has been written and submitted to the Astrophysical Journal.