--=====================_433436358==_.ALT Content-Type: text/plain; charset="us-ascii"; format=flowed HUBBLE SPACE TELESCOPE DAILY REPORT # 3138 PERIOD COVERED: DOY 165-167: 0000Z (UTC) 06/14/02 - 0000Z (UTC) 06/16/02 OBSERVATIONS SCHEDULED:(see HSTARS below for possible observation problems) ACS 9289 Low Redshift Cluster Gravitational Lensing Survey This proposal has two main scientific goals: to determine the dark matter distribution of massive galaxy clusters, and to observe the high redshift universe using these clusters as powerful cosmic telescopes. Deep, g, r, i, z imaging of a sample of low-z {0.2-0.4} clusters will yield a large sample of lensed background galaxies with reliable photometric redshifts. Using multiple pointings with a central overlap region we will reach HDF-like depth in the central, highly magnified cluster region and a shallower but wider coverage in the outer cluster regions. By combining strong and weak lensing constraints with the photometric redshift information it will be possible to precisely measure the cluster dark matter distribution with an unprecedented combination of high spatial resolution and area coverage, avoiding many of the uncertainties which plague ground-based studies and yielding definitive answers about the structure of massive dark matter haloes. In addition, the cosmological parameters can be constrained in a largely model independent way using the multiply lensed objects due to the dependence of the Einsteinng radius on the distance to the source. We can also expect to detect several highly magnified dropout galaxies behind the clusters in the redshift ranges 4-5 5-6 and 7-8, corresponding to a drop in the flux in the g, r, and i bands relative to longer wavelength. We will obtain the best information to date on the giant arcs already known in these clusters, making possible detailed, pixel-by-pixel studies of their star formation rate, dust distribution and structural components, including spiral arms, out to a redshift of around z~2.5 in several passbands. ACS/CAL 9558 ACS weekly Test 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 9391 High-Resolution Imaging of Pluto's Surface We will collect a series of observations with the ACS/HRC from which we will derive a two-color global map of Pluto's surface. We will image Pluto at F435W and F555W, wavelengths that have been extensively studied from the ground over the past 50 years. The maps will provide albedos with accurate error determinations down to 52 degrees South latitude. These observations will provide a second epoch of HST mapping of the active surface of Pluto as it continues to recede from the Sun and will provide an important context for other detailed studies of Pluto. ACS/WFC 9575 Default {Archival} Pure Parallel Program. The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in POMS. ACS/WFC/HRC 8947 Weekly Test. The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to monitor, the read noise, the development of hot pixels and test for any source of noise in ACS CCD detectors. This program will be executed at least once a day for the entire lifetime of ACS. FGS/1 9169 An Interferometric Harvest of Double Degenerates. Fine Guidance Sensor #1R was used to observe the white dwarf mass and age distributions that hold clues to the star formation history of our Galaxy and the age of the disk. NICMOS 9269 NICMOS Parallel Thermal Background NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for the entire duration of SMOV to establish the stability of the HST+NCS+Instrument thermal emission. NICMOS 8790 NICMOS Post-SAA calibration - CR Persistence Part 1. 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. STIS 9618 STIS MAMA Dispersion Solutions Obtain wavecals just deep enough to constrain wavelength and spatial distortion maps without overusing the calibration lamp. For the first time on orbit, data will be obtained at all available central wavelengths. This information will help constrain global models of STIS optical performance being developed at ECF and STScI. During the observations, MSM monthly offsets will be set to zero to complement observations over the past couple of cycles, which occurred at extreme monthly offsets. The echelle observations at zero offset will yield dispersion solutions that are directly applicable to all echelle science data obtained after monthly offsets are disabled. STIS/CCD 8904 Bias Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order to build up high-S/N superbiases and track the evolution of hot columns. STIS/CCD 9066 Closing in on the Hydrogen Reionization Edge of the Universe. The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain the Hydrogen reionization edge in emission that marks the transition from a neutral to a fully ionized IGM at a predicted redshifts. STIS/CCD 8902 Dark Monitor-Part 2. The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks. STIS/CCD 8588 Gamma-Ray Bursts and their Host Environments. The Space Telescope Imaging Spectrograph (CCD) was used to investigate the physics of gamma-ray bursts {GRBs} and the nature of their host galaxies. The approach is three-pronged: 1} rapid HST ultraviolet spectroscopy and Chandra imaging obtained within two days of an outburst will allow probing the physics of the relativistic fireball and the nature of the ISM surrounding the GRB; 2} long-term optical monitoring of the optical transient {OT} will permit testing the hypothesis that GRBs are frequently highly collimated and to determine whether supernovae underlie GRBs; 3} Chandra and HST observations of "dark" GRBs will allow probing one of the greater mysteries surrounding GRBs, the nature of the bursts without optical counterparts. STIS/CCD 9317 Pure Parallel Imaging Program: Cycle 10. The Space Telescope Imaging Spectrograph (CCD) was used to perform the default archival pure parallel program for STIS during cycle 10. STIS/CCD 9136 T Tauri Star Coronagraphic Survey: A PMS Protoplanetary Disk Census. The Space Telescope Imaging Spectrograph (CCD) was used to observe pre-main sequence solar-mass stars, the T Tauri stars that Millimeter and IR studies suggest at least 50 percent have circumstellar disks similar to the disk from which our planetary system formed. High spatial resolution, high dynamic range imaging of such systems will map the spatial distribution of material around the star, constraining the disk sizes and inclinations, and provide a first assessment of when structure in the disk, such as cleared central zones and annuli, which has been linked to planet formation, develops. STIS/CCD 9074 The Origin and Physics of Gamma-Ray Bursts. The Space Telescope Imaging Spectrograph (CCD) was used to make observations that will provide the most stringent tests yet performed of the hypothesis that GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be used to detect broad atomic features of supernovae underlying GRB optical transients, at flux levels more than a factor of three fainter than SN 1998bw. WF/PC-2 9180 Gamma-ray Burst Progenitors: Probing Their Environment. The WF/PC-2 was used to perform a target of opportunity observation of gamma ray burster (GRB), GRB-011121. GRB astronomy is a field maturing at a phenomenal rate. Three important new observational and theoretical discoveries, formulated over the last twelve months, allow the proposer to address new, and in many cases, more sophisticated questions than could have been posed previously. These developments: the discovery of X-ray lines in GRB 991216; the observation that N_H as deduced from X-ray afterglow are one to two orders of magnitude larger than the dust extinction inferred from optical afterglow; and the growing realization that the afterglow emission may exhibit features of dust echoes, appear to offer unexpected and new diagnostics that will directly inform us about the progenitor, the circum-progenitor material and the immediate interstellar environs. WF/PC-2 9319 POMS Test Proposal: WFII Backup Parallel Archive Proposal II. The WF/PC-2 was used to execute a POMS test proposal, designed to simulate future scientific plans. WF/PC-2 9318 POMS Test Proposal: WFII Parallel Archive Proposal Continuation. The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival Pure Parallel program. The program was used to take parallel images of random areas of the sky, following the recommendations of the Parallels Working Group. WFPC2 8938 WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3. This dark calibration program obtains 3 dark frames every day to provide data for monitoring and characterizing the evolution of hot pixels. FLIGHT OPERATIONS SUMMARY: HSTARS: (For details http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf) 8700 - Scheduling Errors in Final Products: SMS168M01 @ 165/0000z Two occurrences of Forward link supports scheduled outside of Return link, one occurrence of SSAT turned on several minutes prior to SSAR service. Under investigation. 8701 - Interface Mean Temperature OOL @ 165/1730z At 165/17:30:59 the mnemonic ICDZ5BMN flagged out of limit red high EV= -5.98429 degC. Red limits L=-46.0 H=-6.0. We were in orbit day and we were not in a SAA. The anomaly happen right after a centering slew and the start of a GSacq.Under investigation. 8702 - EMNBF3T (Main Baffle 3 Temp) Out of Limit Low @ 166/1150z Beginning at 166/11:05:18 the mnemonic EMNBF3T (Main Baffle 3 temperature) flagged intermittently out of limit low with a value of -30.3746 degrees, limit was -30.0. An extract plot shows temperature was steadily decreasing beginning at approximately 165/23:00 and is most likely due to V1-sun angle of 178 degrees and off nominal roll angle of 101 degrees during the period from 165/20:00 to 166/09:11, followed by a V1-sun angle of 135 degrees and off nominal roll angle of 18 degrees during the period beginning at 09:11. On call OTA and TCS engineers were notified. Ops Note 1014-1 was submitted at 13:14 to lower limit to -31.0 degrees at request of TCS SE. Additional intermittent limit violations occurred from 13:20:51 to 14:03:32 with a low value of -31.1859 degrees, no further action was taken to lower limit because the temperature began to increase at 14:03:32 and is no longer violating the revised limit. Ops Note will expire at 174/00:00 after a similar period of high V1-sun angle on day 173. Under investigation. 8703 - GSacq(2,1,2) Results in Fine Lock Backup (2,0,2) @ 166/2333z. The GSacq (2,1,2) of 166/23:33:09 showed Star Selector Cmp Er A flag on FGS2, then resulted in Fine Lock Backup using FGS# 2 (2,0,2). FGS #1 started the walkdown process but was stopped after FGS #2 reached Fine Lock first. No flags remained after the Acquisition completed a and no error message was sent to the 486 STB events record. The following Three REacqs all failed to FLBU on FGS #2 (2,0,2) as well. Under investigation. ******The following science observations may have been affected: ACS 211-229 STIS 141-153 NIC 165-177 WFPC 185-194 8704 - GSacq(1,3,3) Failed to RGA Mode @ 168/0117z. The GSACQ(1,3,3) scheduled at 168/01:17:54 failed to RGA Mode, due to search radius limit exceeded on FGS #1. Primary FGS #1 search radius = 55 a-s. Subsequent MAP at 168/01:55:00 showed vehicle axis errors: v1= -3.244, v2= -2.424, v3= 1.704 (arcsec). This shows that this is not an attitude error. PCS_SE Dan Smith was called. REAcq's(1,3,3) at 168/ 02:54:05, 04:30:14 and 06:06:23 all failed to RGA Mode. Under investigation. *****Observations affected: STIS 2 - 8, WFPCII 3 - 13, ACS 2 - 6, NIC 1 - 12 COMPLETED OPS REQs: 16789-0 - NSSC-1 Memory Dump (ROP NS-2) @ 165/1701z 16790-0 - FHST Map @ 168/0511z OPS NOTES EXECUTED: 1014-1 - Main Baffle 3 limit adjust @ 166/1315z 939-1 - NSSC-1 Load in Count Mode @ 166/2053z SCHEDULED SUCCESSFUL FAILURE TIMES FGS GSacq 13 12 HSTAR 8704 FGS REacq 30 27 HSTAR 8704 FHST Update 34 33 168/0101z LOSS of LOCK None Operations Notes: None SIGNIFICANT EVENTS: Continuation of Servicing Mission Orbital Verification and the gradual resumption of normal science observations and calibrations. --=====================_433436358==_.ALT Content-Type: text/html; charset="us-ascii" HUBBLE SPACE TELESCOPE

DAILY REPORT # 3138

PERIOD COVERED: DOY 165-167: 0000Z (UTC) 06/14/02 - 0000Z (UTC) 06/16/02

OBSERVATIONS SCHEDULED:(see HSTARS below for possible observation problems)

ACS 9289

Low Redshift Cluster Gravitational Lensing Survey

This proposal has two main scientific goals: to determine the dark matter
distribution of massive galaxy clusters, and to observe the high redshift
universe using these clusters as powerful cosmic telescopes. Deep, g, r, i, z
imaging of a sample of low-z {0.2-0.4} clusters will yield a large sample of
lensed background galaxies with reliable photometric redshifts. Using multiple
pointings with a central overlap region we will reach HDF-like depth in the
central, highly magnified cluster region and a shallower but wider coverage in
the outer cluster regions. By combining strong and weak lensing constraints with
the photometric redshift information it will be possible to precisely measure
the cluster dark matter distribution with an unprecedented combination of high
spatial resolution and area coverage, avoiding many of the uncertainties which
plague ground-based studies and yielding definitive answers about the structure
of massive dark matter haloes. In addition, the cosmological parameters can be
constrained in a largely model independent way using the multiply lensed objects
due to the dependence of the Einsteinng radius on the distance to the source. We
can also expect to detect several highly magnified dropout galaxies behind the
clusters in the redshift ranges 4-5 5-6 and 7-8, corresponding to a drop in the
flux in the g, r, and i bands relative to longer wavelength. We will obtain the
best information to date on the giant arcs already known in these clusters,
making possible detailed, pixel-by-pixel studies of their star formation rate,
dust distribution and structural components, including spiral arms, out to a
redshift of around z~2.5 in several passbands.

ACS/CAL 9558

ACS weekly Test

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 9391

High-Resolution Imaging of Pluto's Surface

We will collect a series of observations with the ACS/HRC from which we will
derive a two-color global map of Pluto's surface. We will image Pluto at F435W
and F555W, wavelengths that have been extensively studied from the ground over
the past 50 years. The maps will provide albedos with accurate error
determinations down to 52 degrees South latitude. These observations will
provide a second epoch of HST mapping of the active surface of Pluto as it
continues to recede from the Sun and will provide an important context for other
detailed studies of Pluto.

ACS/WFC 9575

Default {Archival} Pure Parallel Program.

The Advanced Camera for Surveys (WFC) was used to test ACS pure parallels in
POMS.

ACS/WFC/HRC 8947

Weekly Test.

The Advanced Camera for Surveys (WFC and HRC) was used to perform basic tests to
monitor, the read noise, the development of hot pixels and test for any source
of noise in ACS CCD detectors. This program will be executed at least once a day
for the entire lifetime of ACS.

FGS/1 9169

An Interferometric Harvest of Double Degenerates.

Fine Guidance Sensor #1R was used to observe the white dwarf mass and age
distributions that hold clues to the star formation history of our Galaxy and
the age of the disk.

NICMOS 9269

NICMOS Parallel Thermal Background

NICMOS Camera 3 pure parallel exposures in the F222M filter will be obtained for
the entire duration of SMOV to establish the stability of the HST+NCS+Instrument
thermal emission.

NICMOS 8790

NICMOS Post-SAA calibration - CR Persistence Part 1.

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.

STIS 9618

STIS MAMA Dispersion Solutions

Obtain wavecals just deep enough to constrain wavelength and spatial distortion
maps without overusing the calibration lamp. For the first time on orbit, data
will be obtained at all available central wavelengths. This information will
help constrain global models of STIS optical performance being developed at ECF
and STScI. During the observations, MSM monthly offsets will be set to zero to
complement observations over the past couple of cycles, which occurred at extreme
monthly offsets. The echelle observations at zero offset will yield dispersion
solutions that are directly applicable to all echelle science data obtained
after monthly offsets are disabled.

STIS/CCD 8904

Bias Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the bias in
the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4 in order
to build up high-S/N superbiases and track the evolution of hot columns.

STIS/CCD 9066

Closing in on the Hydrogen Reionization Edge of the Universe.

The Space Telescope Imaging Spectrograph (CCD) was used in parallel constrain
the Hydrogen reionization edge in emission that marks the transition from a
neutral to a fully ionized IGM at a predicted redshifts.

STIS/CCD 8902

Dark Monitor-Part 2.

The Space Telescope Imaging Spectrograph (CCD) was used to monitor the darks.

STIS/CCD 8588

Gamma-Ray Bursts and their Host Environments.

The Space Telescope Imaging Spectrograph (CCD) was used to investigate the
physics of gamma-ray bursts {GRBs} and the nature of their host galaxies. The
approach is three-pronged: 1} rapid HST ultraviolet spectroscopy and Chandra
imaging obtained within two days of an outburst will allow probing the physics
of the relativistic fireball and the nature of the ISM surrounding the GRB; 2}
long-term optical monitoring of the optical transient {OT} will permit testing
the hypothesis that GRBs are frequently highly collimated and to determine
whether supernovae underlie GRBs; 3} Chandra and HST observations of "dark" GRBs
will allow probing one of the greater mysteries surrounding GRBs, the nature of
the bursts without optical counterparts.

STIS/CCD 9317

Pure Parallel Imaging Program: Cycle 10.

The Space Telescope Imaging Spectrograph (CCD) was used to perform the default
archival pure parallel program for STIS during cycle 10.

STIS/CCD 9136

T Tauri Star Coronagraphic Survey: A PMS Protoplanetary Disk Census.

The Space Telescope Imaging Spectrograph (CCD) was used to observe pre-main
sequence solar-mass stars, the T Tauri stars that Millimeter and IR studies
suggest at least 50 percent have circumstellar disks similar to the disk from
which our planetary system formed. High spatial resolution, high dynamic range
imaging of such systems will map the spatial distribution of material around the
star, constraining the disk sizes and inclinations, and provide a first
assessment of when structure in the disk, such as cleared central zones and
annuli, which has been linked to planet formation, develops.

STIS/CCD 9074

The Origin and Physics of Gamma-Ray Bursts.

The Space Telescope Imaging Spectrograph (CCD) was used to make observations
that will provide the most stringent tests yet performed of the hypothesis that
GRBs are powered by the collapse of massive stars. STIS CCD spectroscopy will be
used to detect broad atomic features of supernovae underlying GRB optical
transients, at flux levels more than a factor of three fainter than SN 1998bw.

WF/PC-2 9180

Gamma-ray Burst Progenitors: Probing Their Environment.

The WF/PC-2 was used to perform a target of opportunity observation of gamma ray
burster (GRB), GRB-011121. GRB astronomy is a field maturing at a phenomenal
rate. Three important new observational and theoretical discoveries, formulated
over the last twelve months, allow the proposer to address new, and in many
cases, more sophisticated questions than could have been posed previously. These
developments: the discovery of X-ray lines in GRB 991216; the observation that
N_H as deduced from X-ray afterglow are one to two orders of magnitude larger
than the dust extinction inferred from optical afterglow; and the growing
realization that the afterglow emission may exhibit features of dust echoes,
appear to offer unexpected and new diagnostics that will directly inform us
about the progenitor, the circum-progenitor material and the immediate
interstellar environs.

WF/PC-2 9319

POMS Test Proposal: WFII Backup Parallel Archive Proposal II.

The WF/PC-2 was used to execute a POMS test proposal, designed to simulate
future scientific plans.

WF/PC-2 9318

POMS Test Proposal: WFII Parallel Archive Proposal Continuation.

The WF/PC-2 was used to perform the generic target version of the WFPC2 Archival
Pure Parallel program. The program was used to take parallel images of random
areas of the sky, following the recommendations of the Parallels Working Group.

WFPC2 8938

WFPC2 CYCLE 9 SUPPLEMENTAL DARKS pt3/3.

This dark calibration program obtains 3 dark frames every day to provide data
for monitoring and characterizing the evolution of hot pixels. FLIGHT OPERATIONS
SUMMARY:

HSTARS: (For details http://hst-sers.hst.nasa.gov/SERS/HST/HSTAR.nsf)

8700 - Scheduling Errors in Final Products: SMS168M01 @ 165/0000z
       Two occurrences of Forward link supports scheduled outside
       of Return link, one occurrence of SSAT turned on several
       minutes prior to SSAR service. Under investigation.

8701 - Interface Mean Temperature OOL @ 165/1730z
       At 165/17:30:59 the mnemonic ICDZ5BMN flagged out of limit
       red high EV= -5.98429 degC. Red limits L=-46.0 H=-6.0. We were
       in orbit day and we were not in a SAA. The anomaly happen right
       after a centering slew and the start of a GSacq.Under investigation.

8702 - EMNBF3T (Main Baffle 3 Temp) Out of Limit Low @ 166/1150z Beginning
       at 166/11:05:18 the mnemonic EMNBF3T (Main Baffle 3 temperature)
       flagged intermittently out of limit low with a value of -30.3746
       degrees, limit was -30.0. An extract plot shows temperature was
       steadily decreasing beginning at approximately 165/23:00 and is
       most likely due to V1-sun angle of 178 degrees and off nominal roll
       angle of 101 degrees during the period from 165/20:00 to 166/09:11,
       followed by a V1-sun angle of 135 degrees and off nominal roll angle
       of 18 degrees during the period beginning at 09:11. On call OTA and
       TCS engineers were notified. Ops Note 1014-1 was submitted at 13:14
       to lower limit to -31.0 degrees at request of TCS SE. Additional
       intermittent limit violations occurred from 13:20:51 to 14:03:32
       with a low value of -31.1859 degrees, no further action was taken to
       lower limit because the temperature began to increase at 14:03:32
       and is no longer violating the revised limit. Ops Note will expire
       at 174/00:00 after a similar period of high V1-sun angle on day 173.
       Under investigation.

8703 - GSacq(2,1,2) Results in Fine Lock Backup (2,0,2) @ 166/2333z. The
       GSacq (2,1,2) of 166/23:33:09 showed Star Selector Cmp Er A flag on
       FGS2, then resulted in Fine Lock Backup using FGS# 2 (2,0,2). FGS #1
       started the walkdown process but was stopped after FGS #2 reached
       Fine Lock first. No flags remained after the Acquisition completed a
       and no error message was sent to the 486 STB events record.
       The following Three REacqs all failed to FLBU on FGS #2 (2,0,2) as well.
       Under investigation.

       ******The following science observations may have been affected: ACS 211-229
       STIS 141-153 NIC 165-177 WFPC 185-194

8704 - GSacq(1,3,3) Failed to RGA Mode @ 168/0117z. The GSACQ(1,3,3) scheduled
       at 168/01:17:54 failed to RGA Mode, due to search radius limit exceeded
       on FGS #1. Primary FGS #1 search radius = 55 a-s. Subsequent MAP at
       168/01:55:00 showed vehicle axis errors: v1= -3.244, v2= -2.424, v3= 1.704
       (arcsec). This shows that this is not an attitude error. PCS_SE Dan Smith
       was called. REAcq's(1,3,3) at 168/ 02:54:05, 04:30:14 and 06:06:23 all
       failed to RGA Mode. Under investigation.

       *****Observations affected: STIS 2 - 8, WFPCII 3 - 13, ACS 2 - 6,  NIC 1 - 12

COMPLETED OPS REQs:
16789-0 - NSSC-1 Memory Dump (ROP NS-2) @ 165/1701z
16790-0 - FHST Map @ 168/0511z

OPS NOTES EXECUTED:
1014-1 - Main Baffle 3 limit adjust @ 166/1315z
939-1 - NSSC-1 Load in Count Mode @ 166/2053z


                     SCHEDULED     SUCCESSFUL    FAILURE TIMES
FGS GSacq               13               12                     HSTAR 8704
FGS REacq               30                27                    HSTAR 8704
FHST Update             34                33                      168/0101z           
LOSS of LOCK           None                                          



Operations Notes: None

SIGNIFICANT EVENTS:

Continuation of Servicing Mission Orbital Verification and the gradual
resumption of normal science observations and calibrations.
--=====================_433436358==_.ALT--