New version for WFPC2: Ref. Program Change Request 1351 ----- Submission 1 (Wed May 17 01:14:49 GMT 2006) ----- Phase II Proposal 10873 (cyc15_phase2_mkn34_cvz) successfully submitted. ----- Attempting Submission 2 (Thu Mar 15 21:56:33 GMT 2007) ----- Remaining error due to a bug in APT. This has been discussed with our PC, Tony Roman. Submitting as is. Assigned ID: 581 ----- Submission 1 (Fri Jan 27 23:53:36 GMT 2006) ----- Phase I Proposal 581 (cyc15_mkn34) successfully submitted. The Radio-quiet Jet Flow in Markarian 34 The properties of AGN jet flows are notoriously difficult to ascertain. We are currently studying jets in Seyferts by combining emission-line diagnostics with radio observations. We have devised a method of analysis which -- with only modest and reasonable assumptions -- leads to a physical description of the jet flow: its mass, momentum and energy flux, along with its density, velocity and Mach number. We have applied this method to a rich dataset on Markarian 78 and discovered that its jet is very weak, slow, and dense relative to the kind of jets found in radio loud AGN (Whittle \& Wilson 2004, Whittle et al 2005, 2006). Such a difference between radio quiet and radio loud jet flows would be a major result -- if it were found to be generally true. We have more modest observations of a further six Seyferts with jets, but only one of these -- Mkn 34 -- approaches Mkn 78 as a clean enough case to allow our full analysis. Our existing VLA and STIS data are excellent, but the HST archive emission-line and continuum images are of poor quality and low resolution. We are requesting just 3 orbits to obtain higher S/N images at high resolution (ACS/HRC) in [OIII] 5007, [OII] 3727, green and red continuum, bringing the total dataset up to a par with that of Mkn 78. We will then be able to apply our full analysis to determine the nature of the jet flow in this second radio quiet AGN.
This project aims to understand the ionization conditions and jet properties of Mkn 34, by combining ACS imaging and archival STIS spectroscopy of the galaxy nucleus. The central NLR of Mkn 34 extends for about 5 arcsec along the direction of the radio jet-axis and is about 2 arcsec wide at its widest extent. Due to its spatially compact nature and high surface-brightness, we propose to use the ACS/HRC to obtain images of the highest spatial resolution available on HST. We have been awarded 3 orbits of CVZ time for our observing program. Our choice of filters is governed by the need to observe redshifted [OIII] lambda 5007 and [OII] lambda 3727 emission-lines, and suitably associated continuum images. For the emission-line images, we choose the FR388N ([OII]) and FR505N ([OIII]) ramp filters, centered at 3920 and 5266 Angtroms respectively. We have verified that these lines are fully sampled within the 2% bandwidth at the redshift of Mkn 34 (z=0.051). To calculate exposure times, we have used fluxes derived from ground based spectroscopy and the archive HST [OIII] image. Since the ACS ETC does not support the ramp filter configuration, we used nearby narrow band filters to estimate an exposure time of 50 minutes for FR388N and 30 minutes for FR505N to yield peak S/N ratio of ~ 35 per pixel falling to ~ 20 towards the edge of the emission region. The continuum images are needed to a.) subtract the continuum contribution to the ramp filter images, and b.) provide a high S/N dust/reddening map of the Seyfert's nuclear environment. The F550M is an obvious choice to use with the [OIII] ramp filter image -- it excludes all significant emission lines and is sufficiently broad to provide high S/N in relatively short exposure time. In the absence of a fixed-band filter to pair with the [OII] image (the F330W contains Balmer nebular emission which seriously undermines the subtraction process, and F435W contains the redshifted [OII] emission), we will use the FR388N ramp-filter configured to image the line-free continuum around 4000 Angstroms. In addition, the F850LP filter will be used to obtain a high S/N I band image. Paired with the F550M and FR388N continuum images, this will yield a detailed color map. Lastly, a moderately deep wide field ACS-WFC image in F606W will allow the detection of possible signatures of an interaction with a neighbouring galaxy hinted at by ground-based optical imaging studies. Based on ACS ETC calculations with continuum brightnesses measured from our STIS spectra, we estimate a peak S/N ~ 50 per pixel on nucleus dropping to ~ 10 per pixel at the edge of the emission region, for 30 minute exposures in both F550M and F850LP, and an average S/N of ~ 25 for a similar length continuum exposure in FR388N. This is easily adequate for off-band subtraction, but should also yield ratio images which are of sufficient quality to identify any patchy dust features that may in turn be affecting the emission line distribution. A 25 minute exposure in F606W will give complemetary S/N in the outer regions of the galaxy disk. Any early radio outbursts in Mkn 34 should have left their mark in the emission line gas distribution and ionization conditions out to 10-15 arcseconds from the nucleus. Since the emission line surface brightness drops off rapidly beyond the central NLR, reliable construction of ionization and color ratio maps at these distances involves accurate treatment of the background sky emission. By taking a second set of exposures in all HRC filters, but offset by 20 arcseconds (the nuclear FOV of the HRC is not large enough to sample regions outside the host galaxy light distribution), we will be able to accurately correct for this unknown pedestal. While seperate sky images are needed for the FR505N, F550M and F850LP filters, only one sky image for both FR388N images in sufficient, since the background is not expected to vary considerably between their bandpasses. The HRC images will be split in either three or, in the case of the FR388N [OII] image, four subexposures, to limit the effect of cosmic rays. The standard 2-point HRC line dither (integral dither of 5 pixels) will be used for chosen pairs of these subexposures to enable removal of hot pixels, while the WFC image, split into two subexposures, will be offset by a standard 50 pixel line dither pattern to account for the chip gap. Our original Phase I submission proposed for 3 orbits of non-CVZ time. We have been upgraded to 3 orbits of CVZ time, subject to schedulability, after review of a Program Change Request by the Telescope Time Review Board. AGN/QUASARS 12 false 0.0 false false false false false false SUPPORTED GALAXY NLR SEYFERT J2000 10 34 8.6000 +60 01 52.00 J2000 ACS/HRC RampFilter No No FR505N ACS/HRC RampFilter No No FR388N ACS/HRC Imaging No No F550M ACS/HRC Imaging No No F850LP POS-TARG DITHER 0.559017 LINE 0.559017 false false 143.130096 4 26.56505 WFPC2-BOX 1 false POS-TARG DITHER 0.3535 LINE false false 2 45 WFPC2-LINE 2 false /u/rosario/proposals/cyc15_mkn34/OP-cache/cyc15_mkn34_wfpc2_phase2-v01.xml CVZ, redshifted [OII] with quad filter (Tic-Visit :proposal-id 10873 :visit-id "01" :proposal-version -1 :trans-version "20061109" :date "15-Mar-2007 12:46:25.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 3 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 358528 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10873 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :cvz T :proposal-id 10873 :visit-id "01" :orbit-number 1 :pcs-time 355 :si-vis-utilization 16380 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 0 :low-sky "N" :pcs-visibility 0 :pcs-gap 0 ) true 3 0 /tmp/OPVisit9974.xml /u/rosario/proposals/cyc15_mkn34/OP-cache/cyc15_mkn34_wfpc2_phase2-v02.xml [OIII] line and continuum (Tic-Visit :proposal-id 10873 :visit-id "02" :proposal-version -1 :trans-version "20061109" :date "15-Mar-2007 12:54:49.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 448160 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10873 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10873 :visit-id "02" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "02" :orbit-number 2 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "02" :orbit-number 3 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "02" :orbit-number 4 :pcs-time 355 :si-vis-utilization 2840 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "02" :orbit-number 5 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) true 5 0 /tmp/OPVisit10037.xml /u/rosario/proposals/cyc15_mkn34/OP-cache/cyc15_mkn34_wfpc2_phase2-v03.xml [OII] and red continuum (Tic-Visit :proposal-id 10873 :visit-id "03" :proposal-version -1 :trans-version "20061109" :date "15-Mar-2007 13:44:59.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 4 :saa-model "26" :si-bright-earth-limb-angle 20.0 :data-volume 358528 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 10873 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 10873 :visit-id "03" :orbit-number 1 :pcs-time 355 :si-vis-utilization 2840 :al-overhead-at-end 160 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "03" :orbit-number 2 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "03" :orbit-number 3 :pcs-time 355 :si-vis-utilization 2884 :al-overhead-at-end 136 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) (Tic-Orbit :proposal-id 10873 :visit-id "03" :orbit-number 4 :pcs-time 355 :si-vis-utilization 2880 :al-overhead-at-end 180 :internal-dur-at-end 0 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3243 :pcs-gap 0 ) true 4 0 /tmp/OPVisit10046.xml On PC for maximum resolution On WF-ALL for maximum spatial coverage.