Probing Weak Intergalactic Absorption with Flaring Blazar Spectra 2

trying again with CS changes 1930453716 ----- Attempting Submission 5 (Tue Aug 13 19:56:19 GMT 2013) ----- HST Phase II Proposal 13008 (13008_blazar.apt) successfully submitted. ----- Attempting Submission 6 (Tue Aug 13 21:11:26 GMT 2013) ----- ----- Attempting Submission 7 (Tue Dec 10 22:43:45 GMT 2013) ----- ----- Attempting Submission 9 (Thu Dec 12 12:52:27 GMT 2013) ----- All errors are due to generic target #3. Not relevant at this time. Probing Weak Intergalactic Absorption with Flaring Blazar Spectra 2 We propose to exploit the flaring states of high- and unknown-redshift blazars to obtain very high S/N > 25 COS spectra in order to study details of the local intergalactic medium (IGM) not accessible for study using the plethora of lower S/N data being obtained. Only with very high S/N spectra is it possible to detect the weakest Ly alpha and metal lines wherein may lie a substantial portion of the cosmic baryons. The numbers of weak OVI absorbers can discriminate between collisionally ionized and photoionized models, as well as determine which of several galactic outflow models best matches the IGM metal enrichment. Most importantly, high S/N spectra plus the featureless UV power-law continuum of blazars facilitates the detection of broad, shallow absorbers ["broad Ly alpha" (BLA) and broad OVI-only absorbers] which uniquely probe the T = 3 x 10^5 - 3 x 10^6 K range in the IGM where many cosmic baryons are predicted to be "hiding." In addition, these same spectra will be used to obtain lower limits on, or estimates of, the redshift for any featureless blazars observed using the foreground Ly-alpha forest absorbers. In some cases weak Lyman alpha emission may also be detected, as was recently discovered for a few well-known low-redshift BL Lac objects using COS spectra. We request up to three *non-disruptive ToOs* to carry out this program in Cycle 19. Ground-based monitoring will select objects flaring to V ~ 13.5 mag for HST observations, out of a set of about 200 monitored blazars. We have selected our targets from several pools of known blazars. The First group (12) are objects with known or suggested emission redshifts > 0.3 to maximize the pathlength for weak intergalactic Lya, O VI, and other important diagnostic lines. The second group (6) are objects known to be simultaneously bright in TeV gamma-rays and with nominal UV |*|uxes above ~1e-15 erg cm-2 s-1 Ang-1. All targets have measured GALEX NUV and FUV |*|uxes and are in regions of moderate to low Galactic extinction. We assume the unreddened continuum in the optical-UV range follows a power-law be- havior of the form f(nu)=nu^-alpha and determine the slope alpha from published GALEX NUV/FUV fluxes. These fluxes were obtained simultaneously and their ratio should be insensitive to luminosity variations in the AGN. Observed GALEX UV indices are 0 < alpha < 2, typical of those seen in detailed UV spectra of BL Lac objects (e.g., Stocke, Danforth & Perlman 2011). All targets will be monitored on the ground by a network of small, optical telescopes (see Coordinated Observations below) with a ~3 day cadence. We estimate optical trigger thresholds for each target based on these power laws and the observed Galactic extinction toward each object. When the optical magnitude indicates that the reddened |*|ux in the far- UV is ~(2-3)e-14 erg cm-2 s-1 Ang-11, we will activate a non-disruptive ToO observation. The typical magnitude for triggering these observations is V < 13.5. For F1500=3e-14 erg cm-2 s-1 Ang-1, we estimate that we can achieve S/N ~25 per resolution element in a single five-orbit HST visit. The observations will be carried out in both COS/G130M (~2 orbits) and COS/G160M (~3 orbits) using muliple grating central wavelength and FP positions. This is to ensure continuous spectral coverage over the 1132 < lambda < 1795 wavelength range and to dither instrumental features (repellor grid wire shadows, gain sag artifacts, etc.) across the spectrum. Two members of the team have extensive experience in this area as members of the COS GTO team. Unfortunately, we cannot guarantee that any particular object will remain above our flare threshold for the 2-4 weeks required for Preferred Scheduling observations (a.k.a. non- disruptive ToO). To minimize the chances of a miss, we will carefully examine the his- torical variability record for each object and the trend of the flare in progress to predict the duration of a flare. However, even if our chosen blazar has faded somewhat below our F1500~3e-14 erg cm-2 s-1 Ang-1 trigger level, we can still obtain very useful data at lower S/N with our planned observations. As a case in point, 1ES 1553+113 was observed in a non-flaring state (3 HST orbits, F1500~1.5e-14, S/N ~ 15). Danforth et al. (2010) published a study of over 100 intervening absorption lines, including several interesting new OVI absorbers, and constrained the source redshift to 0.3950 < z < 0.45. Even if the objects are not near peak flux during the HST observations, our data (obtained at an above-average flux level) will enable compelling and original science. QUASAR ABSORPTION LINES AND IGM 12 false false 0.0 0.0 false false false SUPPORTED GALAXY BL LAC QSO QUASAR RXJ1001.1+2911 9CJ1001+2911 J2000 F(1300A)~1.5e-14 erg cm-2 s-1 Ang-1 (estimated) GALAXY BL LAC HIGH REDSHIFT GALAXY QSO QUASAR RADIO GALAXY This object was generated by the targetselector and retrieved from the SIMBAD database. VV2010-J234512.4-155507 BZQJ2345-1555 J2000 F(1500A)~1.5e-14 erg cm-2 s-1 Ang-1 GALAXY BL LAC JET QSO QUASAR RADIO GALAXY This object was generated by the targetselector and retrieved from the GSC 2.3 database. PKS1222+216 4C+21.35 J2000 F(1500)~(4+/-2)e-14 erg/cm2/s/Ang COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1300 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1318 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G160M 1611 COS/FUV Spectroscopic No No G160M 1623 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1300 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1318 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G160M 1611 COS/FUV Spectroscopic No No G160M 1623 COS/FUV Spectroscopic No No G130M 1291 COS/FUV Spectroscopic No No G130M 1300 COS/FUV Spectroscopic No No G130M 1309 COS/FUV Spectroscopic No No G130M 1318 COS/FUV Spectroscopic No No G130M 1327 COS/FUV Spectroscopic No No G160M 1577 COS/FUV Spectroscopic No No G160M 1589 COS/FUV Spectroscopic No No G160M 1600 COS/FUV Spectroscopic No No G160M 1611 COS/FUV Spectroscopic No No G160M 1623 The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1386713916105 1366954901000 115.58837661922138 (Tic-Visit :proposal-id 13008 :visit-id "01" :proposal-version -1 :trans-version "20130502" :date "10-Dec-2013 15:18:35.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1157024 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13008 :visit-id "01" :obset-id "01" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13008 :visit-id "01" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2919 :al-overhead-at-end 0 :internal-dur-at-end 67 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "01" :orbit-number 2 :pcs-time 222 :si-vis-utilization 3031 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "01" :orbit-number 3 :pcs-time 222 :si-vis-utilization 3031 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "01" :orbit-number 4 :pcs-time 222 :si-vis-utilization 3031 :al-overhead-at-end 0 :internal-dur-at-end 57 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "01" :orbit-number 5 :pcs-time 222 :si-vis-utilization 3030 :al-overhead-at-end 0 :internal-dur-at-end 385 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3253 :pcs-gap 0 ) true 5 0 S/N>40 at 50% nominal flux or above (F_1500>0.8e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.sa.499016). S/N>40 at 50% nominal flux or above (F_1500>0.8e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.sa.499016). S/N>40 at 50% nominal flux or above (F_1500>0.8e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.sa.499016). For F(1300)=1.6e-14, expect S/N~8 per resel. Buffer time based on 2x nominal count rate. For F(1300)=1.6e-14, expect S/N~8 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1386715386140 ToO observations of PMNJ2345-1555 activated Aug 13, 2013 1377528363000 282.62121812319253 (Tic-Visit :proposal-id 13008 :visit-id "02" :proposal-version -1 :trans-version "20130502" :date "10-Dec-2013 15:43:05.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1296128 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13008 :visit-id "02" :obset-id "02" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13008 :visit-id "02" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2587 :al-overhead-at-end 0 :internal-dur-at-end 114 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "02" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2758 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "02" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2770 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "02" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "02" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2739 :al-overhead-at-end 0 :internal-dur-at-end 376 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) true 5 0 S/N>40 at 50% nominal flux or above (F_1500>1.5e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.ta.196577). For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, we expect S/N~16 per resel. Buffer time based on 2x nominal count rate. The scheduling data was generated by CASM 21.2. CASM was run in Phase II mode. 1386714013817 (Tic-Visit :proposal-id 13008 :visit-id "03" :proposal-version -1 :trans-version "20130502" :date "10-Dec-2013 15:20:13.0" :trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0 :FATAL-ERRORS 0 :CONTINUABLE-FATALS 0) :number-of-orbits 5 :saa-model "31" :si-bright-earth-limb-angle 20.0 :data-volume 1148320 :tdrss-contact-duration 0 :coron NIL ) (Tic-Obset :proposal-id 13008 :visit-id "03" :obset-id "03" :pcs-mode "FGS" ) (Tic-Orbit :proposal-id 13008 :visit-id "03" :orbit-number 1 :pcs-time 333 :si-vis-utilization 2650 :al-overhead-at-end 0 :internal-dur-at-end 124 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "03" :orbit-number 2 :pcs-time 222 :si-vis-utilization 2698 :al-overhead-at-end 0 :internal-dur-at-end 86 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "03" :orbit-number 3 :pcs-time 222 :si-vis-utilization 2740 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "03" :orbit-number 4 :pcs-time 222 :si-vis-utilization 2768 :al-overhead-at-end 0 :internal-dur-at-end 48 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) (Tic-Orbit :proposal-id 13008 :visit-id "03" :orbit-number 5 :pcs-time 222 :si-vis-utilization 2696 :al-overhead-at-end 0 :internal-dur-at-end 376 :dark-offset NIL :dark-utilization 0 :max-dark-utilization 1920 :low-sky "N" :pcs-visibility 3015 :pcs-gap 0 ) false 5 0 S/N>40 at 50% nominal flux or above (F_1500>2e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.sa.548199). S/N>40 at 50% nominal flux or above (F_1500>2e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.sa.548199). S/N>40 at 50% nominal flux or above (F_1500>2e-14). However, if flux is 2x expected level, count rate is still acceptable (COS.sa.548199). For F(1500)=4e-14, we expect S/N~15 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=3e-14, expect S/N~18 per resel. Buffer time based on 2x nominal count rate. For F(1500)=4e-14, we expect S/N~14 per resel. Buffer time based on 2x nominal count rate. For F(1500)=4e-14, we expect S/N~14 per resel. Buffer time based on 2x nominal count rate. For F(1500)=4e-14, we expect S/N~14 per resel. Buffer time based on 2x nominal count rate. For F(1500)=4e-14, we expect S/N~14 per resel. Buffer time based on 2x nominal count rate. For F(1500)=4e-14, we expect S/N~14 per resel. Buffer time based on 2x nominal count rate. For F(1500)=4e-14, we expect S/N~14 per resel. Buffer time based on 2x nominal count rate.