----- Attempting Submission 1 (Fri Oct 24 15:56:18 GMT 2008) ----- We propose to obtain X-ray images and spectra of two of the nearest and X-ray brightest compact symmetric objects. These objects are radio sources which have begun ejecting radio plasma within the last nsim 10000 years. The purpose of these observations is to discover their X-ray structure, measure their X-ray spectra and test the Wilson-Colbert hypothesis regarding the formation of radio-loud AGN. CSOs are ideal targets for this test because they are very small and very young. By targeting the very nearest objects we assure ourselves of the highest possible physical resolution. We are particularly looking for binary black holes (possibly found for one of our objects already) and/or nascent NLRs.

We are obtaining HST images in three bands of the galaxy NGC 5793.We will obtain observations in three bands with HST: F475W and F775W in the optical, using the WFC3 UVIS channel, and F160W in the near-IR, using the WFC3 IR channel. This strategy closely parallels that used in our Cycle 7-N observations of other CSOs, including 4C 31.04, NGC 3894 and 1943+70. The F475W and F775W filters replace the F450W and F702W filters used in our Cycle 7-N program as neither of those is available in WFC3 or ACS. Observing times have been calculated to obtain roughly equal sensitivity in all three bands (H=25.1, i=23.2 and V=23.6 mag/arcsec^2 respectively). The HST data will shed light on such issues as galactic structure, star formation, optical jets, dust features, tidal tails. When viewed in combination with the Chandra and archival radio observations, this will allow us to disentangle how the radio plasma impacts the properties of the gas it flows through as well as the galaxy as a whole. We will also probe the reverse side of the equation -- that is how the galaxy type and other galaxy features affect the evolution of the radio source and the surrounding X-ray atmosphere. Finally for these sources we will probe the deepest inner regions, where the radio source is in the process of taking shape. For NGC 5793 the existing Chandra snapshot shows a double nucleus which we will explore in depth with these HST and deeper Chandra observations. This may be related to the process triggering the ejection of the radio plasma. These observations can be scheduled as flexibly as necessary. We do not have any special requirements as far as roll angle or orbital visibilities; the default parameters will do fine. Also there are no requirements as far as scheduling times. 12 false 0.0 0.0 false false false false false SUPPORTED GALAXY ELLIPTICAL NUCLEUS MULTIPLE NUCLEI RADIO GALAXY LINER This object was generated by the targetselector and retrieved from the NED database. J2000 00 00 0.0000 +00 00 0.00 J2000 POS-TARG DITHER 0.364 LINE false false 2 34.34 WFC3-IR-DITHER-LINE 1 false POS-TARG DITHER 2.391 LINE false false 2 85.248 WFC3-UVIS-DITHER-LINE 2 false The scheduling data was generated by CASM 17.0. CASM was run in Phase II mode. /Users/ericperlman/Documents/OP-cache/11832-v01.xml 1222391818308 (Tic-Visit :proposal-id 11832 :visit-id "01" :proposal-version -1 :trans-version "20071214" :date "25-Sep-2008 21:16:58.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 2 :saa-model "29" :si-bright-earth-limb-angle 20.0 :data-volume 1677232 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 11832 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 11832 :visit-id "01" :orbit-number 1 :pcs-time 365 :si-vis-utilization 2710 :al-overhead-at-end 0 :internal-dur-at-end 90 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) (Tic-Orbit :proposal-id 11832 :visit-id "01" :orbit-number 2 :pcs-time 300 :si-vis-utilization 2953 :al-overhead-at-end 0 :internal-dur-at-end 670 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3257 :pcs-gap 0 ) true 2 0