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Daily 3670
HUBBLE SPACE TELESCOPE - Continuing to collect World Class Science
DAILY REPORT # 3670 PERIOD COVERED: DOYs 219-222 OBSERVATIONS SCHEDULED S/C/NIC1/NIC3 9994 NICMOS Focus Stability The purpose of this activity is to determine if the best focus determined in SMOV is stable. This program will execute in approximately one month intervals starting about 1 month after the last execution of proposal 8980. ACS/WFC 9847 The Structure and Physics of Extragalactic Jets As part of an ongoing investigation into the physics of jets, we propose to obtain ACS polarimetry of the jets of 3C 15, 3C 66B, 3C 346, 3C 371 and PKS 0521-36. This builds on our earlier HST work and completes a sample of 9 jets that spans the range of jet luminosities and morphological types. All of these jets have deep, multi-band HST imaging, and radio polarimetry at matching resolution, and all but one has Chandra data. Our goal is to investigate three fundamental issues, brought to light by recent HST and Chandra observations. These a {1} What is the energetic and magnetic field structure of jets? {2} What is the nature of particle acceleration in jets? {3} What is the nature of the X-ray emission from jets, and what is its relationship to lower energy emissions? Optical polarimetry provides unique information about all of these issues. Because of their vastly different radiative lifetimes {hundreds of years compared to millions}, optical and radio polarimetry probe different electron populations and emission regions. Comparison of radio and optical polarimetry can therefore yield direct information about the three-dimensional energetic and magnetic field structure of jets. Optical polarimetry traces the magnetic field configuration in and near electron acceleration regions, and when combined with optical and X-ray spectral index maps, polarimetry can yield key constraints about particle acceleration and the nature of the X-ray emission of jets. NIC1/NIC2 9844 Brown dwarf atmospheric variability observations We propose to use NIC1 and NIC2 to study brown dwarfs for atmospheric variability. We will observe a sequence of early Ts, a detected variable T2, a T3 and a T4.5. Atmospheric variability, that is expected by some models for these objects, would constrain the physical parameters of cloud vertical distribution, horizontal homogeneity and the dynamics of the very cool atmospheres. The existence and amplitude of the variations would reveal the size and distribution of the cloud cover over the surface of the brown dwarf and test a model explaining the rapidity of the L to T type transition. The relative color changes would constrain the vertical extent of dynamical process and the depth in the atmosphere at which they take place. If a periodicity is measured, the rotational period of the dwarf could be estimated. ACS/HRC 9838 The Upper End of the Supermassive Black Hole Mass Function: Pushing the 10 Billion Solar Mass Limit. In 1994, HST provided the first secure detection of a supermassive black hole {SBH} in a galactic nucleus. The galaxy was M87, the black hole almost 4 billion solar masses. Since then, two dozen additional SBH detections have been the outcome of the several hundred orbits of HST time devoted to this cause. Yet, M87's black hole is still the most massive known, and in only two other galaxies have SBHs in excess of a billion solar masses been detected. The aim of this proposal is to characterize the high mass end of the local SBH mass function. Four brightest cluster galaxies have been carefully selected. Their large masses, luminosites and stellar velocity dispersions, as well as their having a merging history which is unmatched by galaxies in less crowded environments, make these galaxies the most promising hosts of the most massive SBHs in the local Universe. It is in the high mass regime that the unavoidable link between the evolution of supermassive black holes and the hierarchical build-up of galaxies leaves its clearest signature. It is these galaxies that are expected to be the relicts of the most luminous high redshift quasars, those so spectacularly targeted by the Sloan Digital Sky Survey. Expanding {and extending} the high mass end of the local SBH mass function is the next obligatory step we need to take to improve our understanding of how SBHs, and their hosts, formed and evolved. ACS/WFC/WFPC2 9774 Young Massive Clusters in Spiral Galaxies and the Connection with Open Clusters We propose to carry out a census of star clusters in the disks of the nearby spiral galaxies NGC 45, NGC 1313, NGC 4395, NGC 5236 and NGC 7793. Using ACS, we will identify much fainter and older star clusters than possible in previous ground-based surveys, or even in HST imaging of more distant galaxies. For the first time, we will directly explore the connection between young "massive'' {or "super''} star clusters {YMCs} and lower-mass "open'' clusters in different star forming environments. We will test the universality of the luminosity- and mass functions of stellar clusters and establish whether the presence of YMCs is a result of a top-heavy cluster luminosity function, or follows from generally richer cluster systems. Our target galaxies span a range of morphological properties, surface brightness and star formation rate. Some of them are known from ground-based studies to host large numbers of YMCs while others have more modest cluster populations. However, previous ground-based data were restricted to luminous clusters younger than about 500 Myr. Here we will extend the search to clusters formed throughout the entire lifetime of each galaxy and reach clusters with properties typical of the Milky Way open clusters. This will allow us to close the gap between studies of extragalactic and Galactic disk clusters. ACS/WFC 9727 Exploration of the SN Ia Hubble Diagram at z 1.2 In the spirit of a Treasury proposal, we propose to organize, and deliver to the astronomical community, non-proprietary follow-up observations of ~10 Type Ia supernovae at 1z1.7 that are expected to be discovered in a Cycle 12 Treasury proposal. Together with the currently available sample, this would provide a Hubble diagram with over 20 SNe Ia in this redshift range, where it is possible to test the current cosmological model in the epoch of deceleration: If z ~ 0.5 SNe Ia are fainter due to evolution rather than an accelerating expansion, they should continue to get fainter at even higher redshifts. This size sample will show trends and outliers, and permit a more rigorous treatment of the asymmetric amplification distribution from gravitational lensing. This is a key redshift range for the studies of dark energy that will be done with future surveys {and future instruments now being designed}; this dataset will lay the ground-work for these studies by establishing the simple properties of the supernovae in this redshift range, including magnitudes, colors, and timescales. If considered more appropriate, this proposal could be treated as a part of a Treasury or Director's Discretionary program, since the data would be available to everybody immediately, and we would welcome others who would want to work with us on it. ACS/HRC 9703 Coronagraphic Search for Planets around Nearby Stars We will use the HRC coronagraph to search for planets, disks, and exo-zodiacal dust around nearby stars. We have selected the following stars: alpha Cen A and B, tau Ceti, and epsilon Eridani. The observations of each star will be taken at two or more epochs. The observations will be broken into a sequence of short exposures and taken at different roll angles to compensate for "telescope breathing" during the orbit. As a further precaution, the observations will be scheduled after the closest possible nearby pointing in order to minimize thermal changes in the OTA during the first orbit of observations. After matching phases, the PSFs from one star will be subtracted from the other star. NIC1/NIC2/NIC3 8793 NICMOS Post-SAA calibration - CR Persistence Part 4 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. S/C 10358 Guide Star Test for program 10265 ACS/HRC/WFC 10287 Stars in Extended HI Disk Galaxies Half of gas rich galaxies have HI disks extending well beyond their optical extents. This gas is a significant potential fuel repository for future star formation. How can galaxies can store such quantities of ISM without any apparent star formation? These extended gas disks have well maintained velocity dispersions and dynamical structure. What is keeping them warm? Perhaps there is star formation, but at such low levels it is not readily apparent. We have begun investigating this problem by looking for low-level star formation in extended HI disk galaxies. Our first target was the spectacularly dark matter dominated galaxy NGC2915. In this case our hypothesis was proven to be correct. We found indications for low level star formation in two ways. {1} Our ACS WFC images show a noticeable blue plume of stars in the g vs g-V as well as the V vs V-I color magnitude diagrams. The blues stars extend over the full area of the WFC and are highly clumped. {2} Previous deep Halpha images shows a few very faint HII regions near the Holmberg radius. The weakness of the HII regions and the large numbers of blue {B} stars suggests that the IMF is truncated at the upper end compared to typical IMF parameterizations. This could imply that H-alpha surveys underestimate the true star formation rate. Another surprising result of the ACS observations is that the old population also extends well passed the Holmberg radius and includes globular clusters. We propose to observe a second galaxy for this program - NGC4789A {DDO154}. Like NGC2915, it also has HI extending more than five times the Holmberg radius in a fairly well ordered disk. In this case the old stellar population is comparatively weak, and the foreground reddening is much less. This second set of observations will give us a check on the generality of the NGC2915 results. In particular an IMF that does not extend up to O star formation could have major implications for metal production, kinetic energy release and ionization of the intergalactic medium. ACS/HRC 10255 A Never Before Explored Phase Space: Resolving Close White Dwarf / Red Dwarf Binaries We propose an ACS Snapshot imaging survey to resolve a well-defined sample of highly probable white dwarf plus red dwarf close binaries. These candidates were selected from a search for white dwarfs with infrared excess from the 2MASS database. They represent unresolved systems {separations less than approximately 2" in the 2MASS images} and are distributed over the whole sky. Our HST+ACS observations will be sensitive to a separation range {1-20 AU} never before probed by any means. The proposed study will be the first empirical test of binary star parameters in the post-AGB phase. By resolving as few as 20 of our ~100 targets with HST, we will be able to characterize the distribution of orbital semi-major axes and secondary star masses. NIC/NIC3 10226 The NICMOS Grism Parallel Survey We propose to continue managing the NICMOS pure parallel program. Based on our experience, we are well prepared to make optimal use of the parallel opportunities. The improved sensitivity and efficiency of our observations will substantially increase the number of line-emitting galaxies detected. As our previous work has demonstrated, the most frequently detected line is Halpha at 0.7z1.9, which provides an excellent measure of current star formation rate. We will also detect star-forming and active galaxies in other redshift ranges using other emission lines. The grism observations will produce by far the best available Halpha luminosity functions over the crucial--but poorly observed--redshift range where galaxies appear to have assembled most of their stellar mass. This key process of galaxy evolution needs to be studied with IR data; we found that observations at shorter wavelengths appear to have missed a large fraction of the star-formation in galaxies, due to dust reddening. We will also obtain deep F110W and F160W images, to examine the space densities and morphologies of faint red galaxies. In addition to carrying out the public parallels, we will make the fully reduced and calibrated images and spectra available on-line, with some ground-based data for the deepest parallel fields included. ACS/WFC 10210 Groups of Dwarf Galaxies: Pools of Mostly Dark Matter? Within 5 Mpc, there are 6 groups with well-known luminous galaxies but there also appears to be a comparable number of groups containing only dwarfs. If these dwarf entities are truly bound then M/L values are an order of magnitude higher than values found for groups with luminous spiral galaxies. There are theoretical reasons to anticipate that low mass halos may frequently be mostly dark. The dynamical influence of low mass halos is negligible in familiar groups with luminous members. By contrast, a study of the dynamics of `groups of dwarfs' may provide direct evidence of the existence of dark matter potential wells with few baryons. The goal of the present study is to gather detailed information on the 3-D distribution of dwarf galaxies suspected to lie within 7 groups of dwarfs within 5 Mpc. Distances with 7% relative accuracy can be measured with the Tip of the Giant Branch method with ACS and integrations within 1 orbit per target. ACS/HRC 10205 ACS Imagery at the Top of the IMF We shall observe two key massive hot stars to investigate the effects of multiplicity and rotational mixing on their parameters and evolution. {1} The prototype O2 If* star HD 93129A dominates the compact cluster Trumpler 14, one of the ionizing clusters of the Carina Nebula. It has been an anchor point for analyses of the most massive stars. Unexpectedly, it has been resolved as a 55 mas binary by FGS. The derived delta m of 0.9 implies that the companion may be similar to the O3 dwarfs HD 93128 and HD 93129B {3" from A} in Tr 14. Recent radio and X-ray data suggest that the HD 93129A system is a colliding-wind binary. We plan an orbit of very short ACS exposures on this key cluster to obtain resolved multicolor photometry of its crowded inner members for the first time. {2} The recent discovery of a CNO dichotomy among five O2 giants in the Magellanic Clouds provides a new evolutionary diagnostic for the most massive stars, which is related to their initial rotational velocities. The abundance anomalies are seen in the UV wind spectra as well as optical lines. ACS/HRC 10199 The Most Massive Galaxies in the Universe: Double Trouble? We are proposing an HST snapshot survey of 70 objects with velocity dispersion larger than 350 km/s, selected from the Sloan Digital Sky Survey. Potentially this sample contains the most massive galaxies in the Universe. Some of these objects may be superpositions; HST imaging is the key to determining if they are single and massive or if they are two objects in projection. The objects which HST imaging shows to be single objects are interesting because they potentially harbor the most massive black holes, and because their existence places strong constraints on galaxy formation models. When combined with ground based data already in hand, the objects which HST imaging shows are superpositions provide valuable information about interaction rates of early-type galaxies as well as their dust content. They also constrain the allowed parameter space for models of binary gravitational lenses {such models are currently invoked to explain discrepancies in the distribution of lensed image flux ratios and separations}. ACS/HRC 10185 When does Bipolarity Impose itself on the Extreme Mass Outflows from AGB Stars? An ACS SNAPshot Survey Essentially all well-characterized preplanetary nebulae {PPNe} -- objects in transition between the AGB and planetary nebula evolutionary phases - are bipolar, whereas the mass-loss envelopes of AGB stars are strikingly spherical. In order to understand the processes leading to bipolar mass-ejection, we need to know at what stage of stellar evolution does bipolarity in the mass-loss first manifest itself? Our previous SNAPshot surveys of a PPNe sample {with ACS & NICMOS} show that roughly half our targets observed are resolved, with well-defined bipolar or multipolar morphologies. Spectroscopic surveys of our sample confirm that these objects have not yet evolved into planetary nebulae. Thus, the transformation from spherical to aspherical geometries has already fully developed by the time these dying stars have become preplanetary nebulae. From this new and surprising result, we hypothesize that the transformation to bipolarity begins during the very late AGB phase, and happens very quickly, just before, or as the stars are evolving off the AGB. We propose to test this hypothesis quantitatively, through a SNAPshot imaging survey of very evolved AGB stars which we believe are nascent preplanetary nebulae; with our target list being drawn from published lists of AGB stars with detected heavy mass-loss {from millimeter-wave observations}. This survey is crucial for determining how and when the bipolar geometry asserts itself. Supporting kinematic observations using long-slit optical spectroscopy {with the Keck}, millimeter and radio interferometric observations {with OVRO, VLA & VLBA} are being undertaken. The results from this survey {together with our previous work} will allow us to draw general conclusions about the onset of bipolar mass-ejection during late stellar evolution, and will provide crucial input for theories of post-AGB stellar evolution. Our survey will produce an archival legacy of long-standing value for future studies of dying stars. NIC2 10173 Infrared Snapshots of 3CR Radio Galaxies Radio galaxies are an important class of extragalactic objects: they are one of the most energetic astrophysical phenomena and they provide an exceptional probe of the evolving Universe, lying typically in high density regions but well-represented across a wide redshift range. In earlier Cycles we carried out extensive HST observations of the 3CR sources in order to acquire a complete and quantitative inventory of the structure, contents and evolution of these important objects. Amongst the results, we discovered new optical jets, dust lanes, face-on disks with optical jets, and revealed point-like nuclei whose properties support FR-I/BL Lac unified schemes. Here, we propose to obtain NICMOS infrared images of 3CR sources with z0.3 as a major enhancement to an already superb dataset. We aim to deshroud dusty galaxies, study the underlying host galaxy free from the distorting effects of dust, locate hidden regions of star formation and establish the physical characteristics of the dust itself. We will measure frequency and spectral energy distributions of point-like nuclei, expected to be stronger and more prevalent in the IR, seek spectral turnovers in known synchrotron jets and find new jets. We will strongly test unified AGN schemes and merge these data with existing X-ray to radio observations. The resulting database will be an incredibly valuable resource to the astronomical community for years to come. ACS/WFC 10146 Solving the problem of the White Dwarf Cooling Sequence End in M4: an efficient approach The end of the white dwarf {WD} cooling sequence {WDCS} has never been observed, despite the importance that it has in providing an age estimate of old stellar systems, independent from the standard method of the main sequence turn off. The best targets for this investigation are the closest stellar clusters, and, among them, globular clusters are the most interesting ones. Being the oldest stellar aggregates, they allow to probe the advanced WD cooling phases, and the independent age estimate coming from the end of their WDCS has an important cosmological impact. M4 is the best target for this investigation. Despite huge observational efforts, we still miss the end of its WDCS. The ACS camera offers a unique opportunity to identify it. Coupled with already existing observations, we here prove that we can finally reach it with only 10 HST orbits. This is probably the last opportunity we have for a large number of years. The data we are requesting here, will also be used to complete other two programs of great astrophysical impact: the observational detection of the main sequence hydrogen burning limit, and the measurement of the geometrical distance of M4. ACS/WFC 10135 Unveiling the Progenitors and Physics of Cosmic Explosions GRBs and XRFs are clearly highly asymmetric explosions and require a long-lived power source {central engine}. In contrast, nearby core-collapse events are essentially spherical explosions. However, the failure of spherical neutrino driven collapses has led to the idea that asymmetric energy release is essential for the explosion. The recent finding of a Type Ic SN in GRB 030329, the association of the low energy event GRB 980425 with SN 1998bw, the theoretical development discussed above and the rise of collapsar models make it timely to consider whether all these explosions contain engines. Given the uncertainties in theoretical modeling it is clear that observations are needed to guide models. A priori there is little reason to expect connection between the ultra-relativistic jet that powers the GRB and the explosive nucleosynthesis of the ~0.5 solar masses of Nickel-56 that powers the accompanying supernova. We propose a comprehensive program of ACS photometric searches {and measurements} for SNe associated with GRBs and XRFs. In concert, we will undertake ground-based spectroscopy to determine velocity widths, and measure engine parameters from pan-chromatic afterglow observations. Our goal is to produce a comprehensive database of engine and SN physical parameters against which theoretical modeling will be guided. ACS/WFC 10120 The Formation Histories and Dynamical Roles of X-ray Binaries in Globular Clusters Close binaries are fundamental to the dynamical stability and evolution of globular clusters, but large populations have been extremely difficult to identify. Chandra X-ray images provide a revolutionary resource, revealing a few to dozens of low-luminosity X-ray sources in every cluster deeply examined; our own Chandra programs uniformly study these ubiquitous X-ray sources {close binaries and their progeny} in 11 clusters. However, definitive understanding of the nature of the various X-ray subpopulations requires the identification of optical counterparts, and HST is the demonstrated key in these crowded environments. We thus propose a proven, efficient, and uniform, HST multicolor imaging program for optical identifications in 6 of our clusters with Chandra data on-hand, but which lack adequate optical images in the HST archive. The proposed ACS images will permit statistical classifications into the various subtypes: CVs, qLMXBs, BY Dra's/RS CVn's {and MSPs}. A unique aspect of our program is that our clusters span a range of physical properties such as central concentration, cluster size, and mass--essential ingredients in the formation, evolution, and dynamical roles of cluster binaries. Exploiting this range of properties, we have identified a relation that provides the first compelling link between the number of X-ray sources and the predicted stellar encounter frequency in globular cluster cores. But further progress in understanding the details implicit in this relationship {e.g., whether CVs and qLMXBs formed primarily via stellar encounters, while BY Dra's/RS CVn's are mainly primordial binaries} demands uniform optical identifications for multiple clusters, spanning the full range physical properties. WFPC2 10112 HST Observations of Astrophysically Important Visual Binaries This is a continuation of a project begun in Cycle 7 and continued up through Cycle 11. The program consists of annual or biannual WFPC2 or FGS observations of three visual binary stars that will ultimately yield fundamental astrophysical results, once their orbits and masses are determined. Our targets are the following: {1} Procyon {P = 41 yr}, for which our first WFPC2 images yielded an extremely accurate angular separation of the bright F star and its much fainter white-dwarf companion. Combined with ground-based astrometry of the bright star, our observation significantly revised downward the derived masses, and brought Procyon A into excellent agreement with theoretical evolutionary tracks for the first time. With the continued monitoring proposed here, we will obtain masses to an accuracy of better than 1%, providing a testbed for theories of both Sun-like stars and white dwarfs. {2} G 107-70, a close double white dwarf {P = 19 yr} that promises to add two accurate masses to the tiny handful of white-dwarf masses that are directly known from dynamical measurements. {3} Mu Cas {P = 21 yr}, a famous metal-deficient G dwarf for which accurate masses will lead to the stars' helium contents, with cosmological implications. WFPC2 10080 Wavelength Stability of Narrow Band and Linear Ramp Filters Verify the mapping of wavelength as a function of CCD position on LRFs; check for changes in central wavelengths of narrow band filters. WFPC2 10072 WFPC2 CYCLE 12 INTERNAL MONITOR This calibration proposal is the Cycle 12 routine internal monitor for WFPC2, to be run weekly to monitor the health of the cameras. A variety of internal exposures are obtained in order to provide a monitor of the integrity of the CCD camera electronics in both bays {gain 7 and gain 15}, a test for quantum efficiency in the CCDs, and a monitor for possible buildup of contaminants on the CCD windows. WFPC2 10071 WFPC2 CYCLE 12 Supplemental Darks Part 3/3 This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. WFPC2 10068 WFPC2 CYCLE 12 Standard Darks This dark calibration program obtains dark frames every week in order to provide data for the ongoing calibration of the CCD dark current rate, and to monitor and characterize the evolution of hot pixels. Over an extended period these data will also provide a monitor of radiation damage to the CCDs. ACS/HRC/WFC 10061 CCD Daily Monitor This program consists of basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This programme will be executed once a day for the entire lifetime of ACS. ACS/HRC/WFC 10044 ACS internal CTE monitor The charge transfer efficiency {CTE} of the ACS CCD detectors will decline as damage due to on-orbit radiation exposure accumulates. This degradation will be closely monitored at regular intervals, because it is likely to determine the useful lifetime of the CCDs. All the data for this program is acquired using internal targets {lamps} only, so all of the exposures should be taken during Earth occultation time {but not during SAA passages}. This program emulates the ACS pre-flight ground calibration and post-launch SMOV testing {program 8948}, so that results from each epoch can be directly compared. Extended Pixel Edge Response {EPER} and First Pixel Response {FPR} data will be obtained over a range of signal levels for both the Wide Field Channel {WFC}, and the High Resolution Channel {HRC}. FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated.) HSTAR 9507: GS Acquisition (1,2,1) @ 221/02:15:59Z resulted in FL backup (1,0,1) due to SSLE on FGS 2. There were no FHST FM Updates scheduled prior to the acquisition. FHST Map scheduled @ 221/02:53Z showed attitude errors of -12.00, -3.192, and -3.757 arcsec. Under investigation. COMPLETED OPS REQs: 17244-1 - SAFE STIS @ 219/1926z OPS NOTES EXECUTED: 1257-1 - Adjust ACS Error Count Limit @ 220/1639z 1257-1 - Adjust ACS Error Count Limit (closed) @ 222/1641z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 34 34 FGS REacq 21 21 FHST Update 52 52 LOSS of LOCK SIGNIFICANT EVENTS: At Project direction, STIS was commanded from Suspend to Safe Mode @ 219/19:25:48Z (OR 17244-1). Signature appears nominal. EPS SE monitored the expected power reduction, load, and structure currents. Since STIS was safed, input power and temperatures within the instrument have reached their nominal safe mode ranges and have stabilized. SI SEs continue to monitor all available temperatures and Voltages while STIS remains in Safe Mode. Battery 1 Capacity Test scheduled to start 223/10:11Z (OR 17245-2 with attached Battery 1 Capacity test script). Three opportunities to connect SA, Section 1 to Diode Bus B are scheduled to ensure no large trickle discharge in the orbit prior to the capacity test. First opportunity 223/11:04Z, second 223/12:39Z, and third 223/14:16Z. |
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