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- Daily Report #5075 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/858cfca516dc5c27?hl=en
- Daily Report #5076 - 1 messages, 1 author http://groups google com/group/sci astro hubble/t/a5db098dfbe37e20?hl=en
============================================================================== TOPIC: Daily Report #5075
http://groups google com/group/sci astro hubble/t/858cfca516dc5c27?hl=en
== 1 of 1 == Date: Thurs, Apr 15 2010 8:03 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5075
PERIOD COVERED: 5am April 14 - 5am April 15, 2010 (DOY 104/09:00z-105/09:00z)
OBSERVATIONS SCHEDULED
ACS/WFC 11995
CCD Daily Monitor (Part 2)
This program comprises basic tests for measuring the read noise and dark current of the ACS WFC and for tracking the growth of hot pixels The recorded frames are used to create bias and dark reference images for science data reduction and calibration This program will be executed four days per week (Mon, Wed, Fri, Sun) for the duration of Cycle 17 To facilitate scheduling, this program is split into three proposals This proposal covers 320 orbits (20 weeks) from 1 February 2010 to 20 June 2010
ACS/WFC/WFC3/IR 11802
WFC3/IR Observations of Strongly Lensing Clusters
We propose WFC3/IR observations of the massive lensing clusters Abell 1689 and Abell 1703 to constrain the properties of both cluster and background field galaxies The dataset will also help constrain the photometric redshift of A1689-zD1, the bright galaxy candidate at z~7 6
NIC2/WFC3/IR 11548
Infrared Imaging of Protostars in the Orion A Cloud: The Role of Environment in Star Formation
We propose NICMOS and WFC3/IR observations of a sample of 252 protostars identified in the Orion A cloud with the Spitzer Space Telescope These observations will image the scattered light escaping the protostellar envelopes, providing information on the shapes of outflow cavities, the inclinations of the protostars, and the overall morphologies of the envelopes In addition, we ask for Spitzer time to obtain 55-95 micron spectra of 75 of the protostars Combining these new data with existing 3 6 to 70 micron photometry and forthcoming 5-40 micron spectra measured with the Spitzer Space Telescope, we will determine the physical properties of the protostars such as envelope density, luminosity, infall rate, and outflow cavity opening angle By examining how these properties vary with stellar density (i e clusters vs groups vs isolation) and the properties of the surrounding molecular cloud; we can directly measure how the surrounding environment influences protostellar evolution, and consequently, the formation of stars and planetary systems Ultimately, this data will guide the development of a theory of protostellar evolution
STIS/CC 11845
CCD Dark Monitor Part 2
Monitor the darks for the STIS CCD
STIS/CC 11847
CCD Bias Monitor-Part 2
Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns
STIS/CCD/MA2 11568
A SNAPSHOT Survey of the Local Interstellar Medium: New NUV Observations of Stars with Archived FUV Observations
We propose to obtain high-resolution STIS E230H SNAP observations of MgII and FeII interstellar absorption lines toward stars within 100 parsecs that already have moderate or high-resolution far-UV (FUV), 900-1700 A, observations available in the MAST Archive Fundamental properties, such as temperature, turbulence, ionization, abundances, and depletions of gas in the local interstellar medium (LISM) can be measured by coupling such observations Due to the wide spectral range of STIS, observations to study nearby stars also contain important data about the LISM embedded within their spectra However, unlocking this information from the intrinsically broad and often saturated FUV absorption lines of low-mass ions, (DI, CII, NI, OI), requires first understanding the kinematic structure of the gas along the line of sight This can be achieved with high resolution spectra of high-mass ions, (FeII, MgII), which have narrow absorption lines, and can resolve each individual velocity component (interstellar cloud) By obtaining short (~10 minute) E230H observations of FeII and MgII, for stars that already have moderate or high- resolution FUV spectra, we can increase the sample of LISM measurements, and thereby expand our knowledge of the physical properties of the gas in our galactic neighborhood STIS is the only instrument capable of obtaining the required high resolution data now or in the foreseeable future
WFC3/ACS/IR 11584
Resolving the Smallest Galaxies with ACS
An order of magnitude more dwarf galaxies are expected to inhabit the Local Group, based on currently accepted galaxy formation models, than have been observed This discrepancy has been noted in environments ranging from the field to rich clusters, with evidence emerging that lower density regions contain fewer dwarfs per giant than higher density regions, in further contrast to model predictions However, there is no complete census of the faintest dwarf galaxies in any environment The discovery of the smallest and faintest dwarfs is hampered by the limitations in detecting such compact or low surface brightness galaxies, and this is compounded by the great difficulty in determining accurate distances to, or ascertaining group membership for, such faint objects The M81 group provides a powerful means for establishing membership for faint galaxies in a low density region With a distance modulus of 27 8, the tip of the red giant branch (TRGB) appears at I ~ 24, just within the reach of ground based surveys We have completed a 65 square degree survey in the region around M81 with the CFHT/MegaCam Half of our survey was completed before Cycle 16 and we were awarded time with WFPC2 to observe 15 new candidate dwarf galaxy group members in F606W and F814W bands in order to construct color-magnitude diagrams from which to measure accurate TRGB distances and determine star formation and metallicity histories The data obtained show that 8 - 9 of these objects are galaxies at the same distance as M81 In completing our survey, we have discovered an additional 8 candidate galaxies we propose to image with ACS in order to measure TRGB distances and establish membership We also wish to re-observe our smallest candidate group member and a tidal dwarf candidate with deeper observations made possible with ACS Once membership has been established for this second set of candidates, we will have a complete census of the dwarf galaxy population in the M8 group to M_r ~ -10, allowing us to obtain a firm measurement of the luminosity function faint-end slope, and, combined with previous HST data, to provide a complete inventory of the age and abundance properties for the collapsed core of the M81 group
WFC3/UVIS 11905
WFC3 UVIS CCD Daily Monitor
The behavior of the WFC3 UVIS CCD will be monitored daily with a set of full-frame, four-amp bias and dark frames A smaller set of 2Kx4K subarray biases are acquired at less frequent intervals throughout the cycle to support subarray science observations The internals from this proposal, along with those from the anneal procedure (Proposal 11909), will be used to generate the necessary superbias and superdark reference files for the calibration pipeline (CDBS)
WFC3/UVIS/IR 11662
Improving the Radius-Luminosity Relationship for Broad-Lined AGNs with a New Reverberation Sample
The radius-luminosity (R-L) relationship is currently the fundamental basis for all techniques used to estimate black hole masses in AGNs, in both the nearby and distant universe However, the current R-L relationship is based on 34 objects that cover a limited range in black hole mass and luminosity To improve our understanding of black hole growth and evolution, the R-L relationship must be extended to cover a broader range of black hole masses using the technique known as reverberation mapping To this end, we have been awarded an unprecedented 64 nights on the Lick Observatory 3-m telescope between March 24 and May 31, 2008, to spectroscopically monitor 12 AGNs in order to measure their black hole masses To properly determine the luminosities of these 12 AGNs, we must correct them for their host-galaxy starlight contributions using high-resolution images Previous work by Bentz et al (2006) has shown that the starlight correction to AGN luminosity measurements is an essential component to interpreting the R-L relationship The correction will be substantial for each of the 12 sources we will monitor, as the AGNs are relatively faint and embedded in nearby, bright galaxies Starlight corrections are not possible with ground-based images, as the PSF and bulge contributions become indistinguishable under typical seeing conditions, and adaptive optics are not yet operational in the spectral range where the corrections are needed In addition, spectral decompositions are very model-dependent and are limited by the degree of accuracy to which we understand emission processes and stellar populations in galaxies Without correcting for starlight, we will be unable to apply the results of our Spring 2008 campaign to the body of knowledge from previous reverberation mapping work Therefore, we propose to obtain high resolution, high dynamic range images of the host galaxies of the 12 AGNs in our ground-based monitoring sample, as well as one white dwarf which will be used as a PSF model
STIS/CCD 11849
STIS CCD Hot Pixel Annealing
This purpose of this activity is to repair radiation induced hot pixel damage to the STIS CCD by warming the CCD to the ambient instrument temperature and annealing radiation damaged pixels Radiation damage creates hot pixels in the STIS CCD Detector Many of these hot pixels can be repaired by warming the CCD from its normal operating temperature near -83 C to the ambient instrument temperature (~ +5 C) for several hours The number of hot pixels repaired is a function of annealing temperature The effectiveness of the CCD hot pixel annealing process is assessed by measuring the dark current behavior before and after annealing and by searching for any window contamination effects
FLIGHT OPERATIONS SUMMARY:
Significant Spacecraft Anomalies: (The following are preliminary reports of potential non-nominal performance that will be investigated )
HSTARS:
12247 - STIS CCD Dark Image Shifted One Column to the Left
The STIS Science Team has reported the one dark science image taken on 2010/003/13:37:00 000 for Proposal 11849 - STIS CCD Hot Pixel Annealing
COMPLETED OPS REQUEST: (None)
COMPLETED OPS NOTES: (None)
SCHEDULED SUCCESSFUL
FGS GSAcq 12 12 FGS REAcq 8 8 OBAD with Maneuver 6 6
SIGNIFICANT EVENTS: (None)
============================================================================== TOPIC: Daily Report #5076
http://groups google com/group/sci astro hubble/t/a5db098dfbe37e20?hl=en
== 1 of 1 == Date: Fri, Apr 16 2010 8:43 am From: "Cooper, Joe"
HUBBLE SPACE TELESCOPE - Continuing to Collect World Class Science
DAILY REPORT #5076
PERIOD COVERED: 5am April 15 - 5am April 16, 2010 (DOY 105/09:00z-106/09:00z)
OBSERVATIONS SCHEDULED
COS/FUV 11541
COS-GTO: Cool, Warm, and Hot Gas in the Cosmic Web and in Galaxy Halos
COS G130M and G160M 20, 000 resolution observations will be obtained for 17 QSOs to study cool, warm and hot gas in the cosmic web and in galaxy halos 5 QSOs with z from 0 177 to 0 574 and sum z = 1 68 will be observed with S/N = 40-50 per resolution element 12 QSOs with z = 0 286 to 0 669 and sum z = 5 57 will be observed with S/N = 30-40 The observations will allow a wide range of IGM studies including determining the frequency of occurrence of the different types of absorption systems detected, along with studies of the physical conditions and elemental abundances in the different systems Special emphasis will be given to a study of the properties of highly ionized IGM as traced by O VI, O V, O IV, N V, and C IV The high S/N of the observations will allow a search for broad Lyman alpha absorption and weak metal line absorption that can be crucial for the evaluation of physical conditions and elemental abundances Supporting ground based observations will allow studies of the association of the absorbers with galaxy structures along the 17 lines of sight The overall goal of the program will be to obtain the information that will allow an assessment of the baryonic content of the IGM as revealed by UV and EUV absorption lines seen in the spectra of QSOs
FGS 11789
An Astrometric Calibration of Population II Distance Indicators
In 2002, HST produced a highly precise parallax for RR Lyrae That measurement resulted in an absolute magnitude, M(V)= 0 61+/-0 11, a useful result, judged by the over ten refereed citations each year since It is, however, unsatisfactory to have the direct, parallax-based, distance scale of Population II variables based on a single star We propose, therefore, to obtain the parallaxes of four additional RR Lyrae stars and two Population II Cepheids, or W Vir stars The Population II Cepheids lie with the RR Lyrae stars on a common K-band Period-Luminosity relation Using these parallaxes to inform that relationship, we anticipate a zero point error of 0 04 magnitude This result should greatly strengthen confidence in the Population II distance scale and increase our understanding of RR Lyrae star and Pop II Cepheid astrophysics
STIS/CC 11845
CCD Dark Monitor Part 2
Monitor the darks for the STIS CCD
STIS/CC 11847
CCD Bias Monitor-Part 2
Monitor the bias in the 1x1, 1x2, 2x1, and 2x2 bin settings at gain=1, and 1x1 at gain = 4, to build up high-S/N superbiases and track the evolution of hot columns
WFC3/ACS/IR 11600
Star Formation, Extinction, and Metallicity at 0
7 The global star formation rate (SFR) is ~10x higher at z=1 than today
This could be due to drastically elevated SFR in some fraction of
galaxies, such as mergers with central bursts, or a higher SFR across
the board
Either means that the conditions in z=1 star forming
galaxies could be quite different from local objects
The next step
beyond measuring the global SFR is to determine the dependence of SFR,
obscuration, metallicity, and size of the star-forming region on
galaxy mass and redshift
However, SFR indicators at z=1 typically
apply local calibrations for UV, [O II] and far-IR, and do not agree
with each other on a galaxy-by-galaxy basis
Extinction, metallicity,
and dust properties cause uncontrolled offsets in SFR calibrations
The great missing link is Balmer H-alpha, the most sensitive probe of
SFR
We propose a slitless WFC3/G141 IR grism survey of GOODS-N, at 2
orbits/pointing
It will detect Ha+[N II] emission from 0
7 WFC3/ACS/UVIS/IR 11570 Narrowing in on the Hubble Constant and Dark Energy A measurement of the Hubble constant to a precision of a few percent
would be a powerful aid to the investigation of the nature of dark
energy and a potent "end-to end" test of the present cosmological
model
In Cycle 15 we constructed a new streamlined distance ladder
utilizing high- quality type Ia supernova data and observations of
Cepheids with HST in the near-IR to minimize the dominant sources of
systematic uncertainty in past measurements of the Hubble constant and
reduce its total uncertainty to a little under 5%
Here we propose to
exploit this new route to reduce the remaining uncertainty by more
than 30%, translating into an equal reduction in the uncertainty of
the equation of state of dark energy
We propose three sets of
observations to reach this goal: a mosaic of NGC 4258 with WFC3 in
F160W to triple its sample of long period Cepheids, WFC3/F160W
observations of the 6 ideal SN Ia hosts to triple their samples of
Cepheids, and observations of NGC 5584 the host of a new SN Ia, SN
2007af, to discover and measure its Cepheids and begin expanding the
small set of SN Ia luminosity calibrations
These observations would
provide the bulk of a coordinated program aimed at making the
measurement of the Hubble constant one of the leading constraints on
dark energy
WFC3/UVIS 11588 Galaxy-Scale Strong Lenses from the CFHTLS Survey We aim to investigate the origin and evolution of early-type galaxies
using gravitational lensing, modeling the mass profiles of objects
over a wide range of redshifts
The low redshift (z = 0
2) sample is
already in place following the successful HST SLACS survey; we now
propose to build up and analyze a sample of comparable size (~50
systems) at high redshift (0
4 < z < 0
9) using HST WFC3 Snapshot
observations of lens systems identified by the SL2S collaboration in
the CFHT legacy survey
WFC3/UVIS 11594 A WFC3 Grism Survey for Lyman Limit Absorption at z=2 We propose to conduct a spectroscopic survey of Lyman limit absorbers
at redshifts 1
8 < z < 2
5, using WFC3 and the G280 grism
This
proposal intends to complete an approved Cycle 15 SNAP program
(10878), which was cut short due to the ACS failure
We have selected
64 quasars at 2
3 < z < 2
6 from the Sloan Digital Sky Survey
Spectroscopic Quasar Sample, for which no BAL signature is found at
the QSO redshift and no strong metal absorption lines are present at z 2
3 along the lines of sight
The survey has three main
observational goals
First, we will determine the redshift frequency
dn/dz of the LLS over the column density range 16
0 < log(NHI) < 20
3
cm^-2
Second, we will measure the column density frequency
distribution f(N) for the partial Lyman limit systems (PLLS) over the
column density range 16
0 < log(NHI) < 17
5 cm^-2
Third, we will
identify those sightlines which could provide a measurement of the
primordial D/H ratio
By carrying out this survey, we can also help
place meaningful constraints on two key quantities of cosmological
relevance
First, we will estimate the amount of metals in the LLS
using the f(N), and ground based observations of metal line
transitions
Second, by determining f(N) of the PLLS, we can constrain
the amplitude of the ionizing UV background at z~2 to a greater
precision
This survey is ideal for a snapshot observing program,
because the on-object integration times are all well below 30 minutes,
and follow-up observations from the ground require minimal telescope
time due to the QSO sample being bright
WFC3/UVIS 11650 Mutual Orbits, Colors, Masses, and Bulk Densities of 3 Cold Classical
Trans-Neptunian Binaries Many Trans-Neptunian Objects (TNOs) have been found to be binary or
multiple systems
As in other astrophysical settings, Trans-Neptunian
Binaries (TNBs) offer uniquely valuable information
Their mutual
orbits allow the direct determination of their system masses, perhaps
the most fundamental physical quantity of any astronomical object
Their frequency of occurrence and dynamical characteristics provide
clues to formation conditions and evolution scenarios affecting both
the binaries and their single neighbors
Combining masses with sizes,
bulk densities can be measured
Densities constrain bulk composition
and internal structure, key clues to TNO origins and evolution over
time
Several TNB bulk densities have been determined, hinting at
interesting trends
But none of them belongs to the Cold Classical
sub-population, the one group of TNOs with demonstrably distinct
physical characteristics
Two top-priority Spitzer programs will soon
observe and measure the sizes of 3 Cold Classical TNBs
This proposal
seeks to determine the mutual orbits and thus masses of these systems,
enabling computation of their densities
WFC3/UVIS 11905 WFC3 UVIS CCD Daily Monitor The behavior of the WFC3 UVIS CCD will be monitored daily with a set
of full-frame, four-amp bias and dark frames
A smaller set of 2Kx4K
subarray biases are acquired at less frequent intervals throughout the
cycle to support subarray science observations
The internals from
this proposal, along with those from the anneal procedure (Proposal
11909), will be used to generate the necessary superbias and superdark
reference files for the calibration pipeline (CDBS)
WFC3/UVIS 11908 Cycle 17: UVIS Bowtie Monitor Ground testing revealed an intermittent hysteresis type effect in the
UVIS detector (both CCDs) at the level of ~1%, lasting hours to days
Initially found via an unexpected bowtie-shaped feature in flatfield
ratios, subsequent lab tests on similar e2v devices have since shown
that it is also present as simply an overall offset across the entire
CCD, i
e
, a QE offset without any discernable pattern
These lab
tests have further revealed that overexposing the detector to count
levels several times full well fills the traps and effectively
neutralizes the bowtie
Each visit in this proposal acquires a set of
three 3x3 binned internal flatfields: the first unsaturated image will
be used to detect any bowtie, the second, highly exposed image will
neutralize the bowtie if it is present, and the final image will allow
for verification that the bowtie is gone
FLIGHT OPERATIONS SUMMARY: Significant Spacecraft Anomalies: (The following are preliminary
reports of potential non-nominal performance that will be
investigated
) HSTARS: (None) COMPLETED OPS REQUEST: (None) COMPLETED OPS NOTES: (None) FGS GSAcq 7 7
FGS REAcq 4 4
OBAD with Maneuver 4 4 SIGNIFICANT EVENTS: (None) ============================================================================== You received this message because you are subscribed to the Google Groups "sci
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