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Daily Rpt #4649
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT*** #4649 PERIOD COVERED: 5am July 9 - 5am July 10, 2008 (DOY 191/0900z-192/0900z) OBSERVATIONS SCHEDULED NIC1/NIC2/NIC3 11318 NICMOS Cycle 16 Multiaccum Darks The purpose of this proposal is to monitor the dark current, read noise, and shading profile for all three NICMOS detectors throughout the duration of Cycle 16. This proposal is a slightly modified version of proposal 10380 of cycle 13 and 9993 of cycle12 and is the same as Cycle 15. Covers the period from April 08 to November 08 (inclusive) NIC1/NIC2/NIC3 11330 NICMOS Cycle 16 Extended Dark This takes a series of Darks in parallel to other instruments. NIC1/NIC2/NIC3 8795 NICMOS Post-SAA Calibration - CR Persistence Part 6 A new procedure proposed to alleviate the CR-persistence problem of NICMOS. Dark frames will be obtained immediately upon exiting the SAA contour 23, and every time a NICMOS exposure is scheduled within 50 minutes of coming out of the SAA. The darks will be obtained in parallel in all three NICMOS Cameras. The POST-SAA darks will be non-standard reference files available to users with a USEAFTER date/time mark. The keyword 'USEAFTER=date/time' will also be added to the header of each POST-SAA DARK frame. The keyword must be populated with the time, in addition to the date, because HST crosses the SAA ~8 times per day so each POST-SAA DARK will need to have the appropriate time specified, for users to identify the ones they need. Both the raw and processed images will be archived as POST-SAA DARKSs. Generally we expect that all NICMOS science/calibration observations started within 50 minutes of leaving an SAA will need such maps to remove the CR persistence from the science images. Each observation will need its own CRMAP, as different SAA passages leave different imprints on the NICMOS detectors. NIC2 11237 The Origin of the Break in the AGN Luminosity Function We propose to use NICMOS imaging to measure rest-frame optical luminosities and morphological properties of a complete sample of faint AGN host galaxies at redshifts z ~ 1.4. The targets are drawn from the VLT-VIMOS Deep Survey, and they constitute a sample of the lowest luminosity type 1 AGN known at z 1. The spectroscopically estimated black hole masses are up to an order of magnitude higher than expected given their nuclear luminosities, implying highly sub-Eddington accretion rates. This exactly matches the prediction made by recent theoretical models of AGN evolution, according to which the faint end of the AGN luminosity function is populated mainly by big black holes that have already exhausted a good part of their fuel. In this proposal we want to test further predictions of that hypothesis, by focusing on the host galaxy properties of our low-luminosity, low- accretion AGN. If the local ratio between black hole and bulge masses holds at least approximately at these redshifts, one expects most of these low-luminosity AGN to reside in fairly big ellipticals with stellar masses around and above 10^11 solar masses (in contrast to the Seyfert phenomenon in the local universe). With NICMOS imaging we will find out whether that is true, implying also a sensitive test for the validity of the M_BH/M_bulge relation at z ~ 1.4. NIC2 11547 Characterizing Pre-Main Sequence Populations in Stellar Associations of the Large Magellanic Cloud The Large Magellanic Cloud (LMC) offers an extremely rich sample of resolved low-mass stars (below 1 Solar Mass) in the act of formation that has not been explored sufficiently yet. These pre-main sequence (PMS) stars provide a unique snapshot of the star formation process, as it is being recorded for the last ~20 Myr, and they give important information on the low-mass Initial Mass Function (IMF) of their host stellar systems. Studies of young, rich LMC clusters like 30 Doradus are crowding limited, even at the angular resolution facilitated by HST in the optical. To learn more about low-mass PMS stars in the LMC, one has to study less crowded regions like young stellar assocations. We propose to employ WFPC2 to obtain deep photometry (V ~ 25.5 mag) of four selected LMC stellar associations in order to perform an original optical analysis of their red PMS and blue bright MS stellar populations. With these observations we aim at a comprehensive study, which will add substantial information on the most recent star formation and the IMF in the LMC. The data reduction and analysis will be performed with a 2D photometry software package especially developped by us for WFPC2 imaging of extended stellar associations with variable background. Our targets have been selected optimizing a combination of criteria, namely spatial resolution, crowding, low extinction, nebular contamination, and background confusion in comparison to other regions in the Local Group. Parallel NICMOS imaging will provide additional information on near-infrared properties of the stellar population in the regions surrounding these systems. NIC2 11799 NICMOS Non-linearity Calibration for Faint Objects NICMOS has played a key role in probing the deep near infrared regime for a decade. It has been the only instrument available to observe objects in the near infrared that are not visible from the ground. In particular, it has played a major role in the SN Ia observations at redshifts z1. However, the calibration of NICMOS has turned out to be difficult due to the apparent non-linearity of the detectors. The NICMOS calibration team has described the non-linearity as a power law based on data in the range of ~50-5000 ADU/s. The correction relies on an extrapolation of two orders of magnitude in flux at count rates close to the sky level (0.1 ADU/s) where space observations are particularly prized - and where SN Ia observations are made. Precise measurements of faint objects require us to reduce the uncertainties from this extrapolation. Here we propose to derive the absolute calibration in the sky limited regime and to characterize the non-linearity over the entire dynamic range for the camera/filter combination: NIC2/F110W. NIC2/WFPC2 11142 Revealing the Physical Nature of Infrared Luminous Galaxies at 0.3z2.7 Using HST and Spitzer We aim to determine physical properties of IR luminous galaxies at 0.3z2.7 by requesting coordinated HST/NIC2 and MIPS 70um observations of a unique, 24um flux-limited sample with complete Spitzer mid-IR spectroscopy. The 150 sources investigated in this program have S{24um} 0.8mJy and their mid-IR spectra have already provided the majority targets with spectroscopic redshifts {0.3z2.7}. The proposed 150~orbits of NIC2 and 66~hours of MIPS 70um will provide the physical measurements of the light distribution at the rest-frame ~8000A and better estimates of the bolometric luminosity. Combining these parameters together with the rich suite of spectral diagnostics from the mid-IR spectra, we will {1} measure how common mergers are among LIRGs and ULIRGs at 0.3z2.7, and establish if major mergers are the drivers of z1 ULIRGs, as in the local Universe. {2} study the co-evolution of star formation and blackhole accretion by investigating the relations between the fraction of starburst/AGN measured from mid-IR spectra vs. HST morphologies, L{bol} and z. {3} obtain the current best estimates of the far-IR emission, thus L{bol} for this sample, and establish if the relative contribution of mid-to-far IR dust emission is correlated with morphology {resolved vs. unresolved}. WEPC2 11196 An Ultraviolet Survey of Luminous Infrared Galaxies in the Local Universe At luminosities above 10^11.4 L_sun, the space density of far-infrared selected galaxies exceeds that of optically selected galaxies. These Luminous Infrared Galaxies {LIRGs} are primarily interacting or merging disk galaxies undergoing starbursts and creating/fueling central AGN. We propose far {ACS/SBC/F140LP} and near {WFPC2/PC/F218W} UV imaging of a sample of 27 galaxies drawn from the complete IRAS Revised Bright Galaxy Sample {RBGS} LIRGs sample and known, from our Cycle 14 B and I-band ACS imaging observations, to have significant numbers of bright {23 B 21 mag} star clusters in the central 30 arcsec. The HST UV data will be combined with previously obtained HST, Spitzer, and GALEX images to {i} calculate the ages of the clusters as function of merger stage, {ii} measure the amount of UV light in massive star clusters relative to diffuse regions of star formation, {iii} assess the feasibility of using the UV slope to predict the far-IR luminosity {and thus the star formation rate} both among and within IR-luminous galaxies, and {iv} provide a much needed catalog of rest- frame UV morphologies for comparison with rest-frame UV images of high-z LIRGs and Lyman Break Galaxies. These observations will achieve the resolution required to perform both detailed photometry of compact structures and spatial correlations between UV and redder wavelengths for a physical interpretation our IRX-Beta results. The HST UV data, combined with the HST ACS, Spitzer, Chandra, and GALEX observations of this sample, will result in the most comprehensive study of luminous starburst galaxies to date. WFPC2 11235 HST NICMOS Survey of the Nuclear Regions of Luminous Infrared Galaxies in the Local Universe At luminosities above 10^11.4 L_sun, the space density of far-infrared selected galaxies exceeds that of optically selected galaxies. These `luminous infrared galaxies' {LIRGs} are primarily interacting or merging disk galaxies undergoing enhanced star formation and Active Galactic Nuclei {AGN} activity, possibly triggered as the objects transform into massive S0 and elliptical merger remnants. We propose NICMOS NIC2 imaging of the nuclear regions of a complete sample of 88 L_IR 10^11.4 L_sun luminous infrared galaxies in the IRAS Revised Bright Galaxy Sample {RBGS: i.e., 60 micron flux density 5.24 Jy}. This sample is ideal not only in its completeness and sample size, but also in the proximity and brightness of the galaxies. The superb sensitivity and resolution of NICMOS NIC2 on HST enables a unique opportunity to study the detailed structure of the nuclear regions, where dust obscuration may mask star clusters, AGN and additional nuclei from optical view, with a resolution significantly higher than possible with Spitzer IRAC. This survey thus provides a crucial component to our study of the dynamics and evolution of IR galaxies presently underway with Wide-Field, HST ACS/WFC and Spitzer IRAC observations of these 88 galaxies. Imaging will be done with the F160W filter {H-band} to examine as a function of both luminosity and merger stage {i} the luminosity and distribution of embedded star clusters, {ii} the presence of optically obscured AGN and nuclei, {iii} the correlation between the distribution of 1.6 micron emission and the mid-IR emission as detected by Spitzer IRAC, {iv} the evidence of bars or bridges that may funnel fuel into the nuclear region, and {v} the ages of star clusters for which photometry is available via ACS/WFC observations. The NICMOS data, combined with the HST ACS, Spitzer, and GALEX observations of this sample, will result in the most comprehensive study of merging and interacting galaxies to date. WFPC2 11498 2008 Passage of Jupiter's Great Red Spot and Oval BA Jupiter's largest anticyclonic storm, the Great Red Spot (GRS), drifts slowly westward relative to the radio rotation rate of the planet (System III W. longitude). In contrast, the next largest storm, Oval BA (a.k.a. the Little Red Spot or LRS), drifts slowly eastward. The relative drift of the two is approximately 0.5 deg/day, resulting in a passage of the storms every two years. The GRS sits at ~22 deg. S planetographic latitude, while the LRS resides at ~33 deg. S latitude. Both vortices deflect nearby eastward and westward winds jets around their periphery, and are somewhat confined to their latitude bands by the alternating, and nearly constant, zonal wind field. However, they do oscillate slightly in latitude, particularly near the times of a passage, in part because the deflected wind jets push to keep the spots separated. It is during these passages that the LRS, and its predecessor white ovals, is most likely to show changes in size and morphology, which are related to the internal wind fields and regulate the vertical cloud structure of the vortex. For example, GRS passages in 1998 and 2000 preceded the merger of the three white ovals into the single large Oval BA, after the ovals and intervening cyclonic cells were deflected by the GRS. We propose to study the 2008 passage to look for changes in internal vortex winds, nearby zonal winds and vortex upper cloud structure, particularly in particle size and opacity, using five orbits of WFPC2 and two orbits of NICMOS. These data will be combined with a multitude of planned ground-based coverage to offer an unprecedented view of a GRS/Oval passage, which will give insight on cloud structure, dynamics, and possibly even water abundance below the cloud decks (water abundance governs the distance of interaction between the two spots). HST is required to provide adequate spatial resolution and wavelength coverage while observing the passage. The 2008 passage is expected to be especially important, as Jupiter underwent a global upheaval in 2007, with disturbances near the GRS and LRS. This upheaval began after the normal Cycle 16 proposal deadline, raising the priority of these observations enough to warrant a request for HST time. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTARS: 11382 NICMOS Suspended @191/19:29z. At 191/19:42:31z (AOS), NICMOS was suspended with a status buffer message NICMOS 632 ("MECH_2_MAX_RETRIES_EXCEEDED"), parameter =172, time = 38986 (19:29:53z), indicating the # of Filter Wheel 2 positioning error retries exceeded the maximum limit. (Ref HSTAR# 11367). Possible Observations affected: NICMOS #135-152 Proposal ID#08795 COMPLETED OPS REQUEST: 18247-0 NICMOS memory dump after suspend @ 191/2225z (HSTAR 11382). 18248-0 NICMOS Suspend Recovery @ 192/0938z (HSTAR 11382). COMPLETED OPS NOTES: (None) ********************************* SCHEDULED***** SUCCESSFUL FGS GSacq************************* 8******************** 8 FGS REacq************************* 4******************** 4 OBAD with Maneuver********** ** ** 24****************** 24 SIGNIFICANT EVENTS: NICMOS suspended today at D191/19:29:53 (3:29pm eastern time) due to filter wheel #2 exceeding its maximum allotted number of retries (HSTAR 11382). This is believed to be the same type of event that occurred on June 30, 2008 (HSTAR 11367). The current recovery plan is as follows: 191/22:16 - Ops Req. 18247 NICMOS Memory Dump after Suspend. Completed @ 191/2225z. At ~192/09:30 - Ops Req. #18248 NICMOS Suspend Recovery. NICMOS successfully recovered from suspend to SAA Operate via Ops Request 18248-0 at 09:38z this morning.* The transition from SAA Operate to Observe occurred via scheduled SMS commanding at 09:57z and the first internal observation successfully started at 10:00z. |
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