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Assigned ID: 127
----- Attempting Submission 1 (Tue Mar 03 19:53:02 GMT 2020) -----
HST Phase I Proposal 127 successfully submitted.
Receipt: # 127-1
----- Attempting Submission 2 (Fri Mar 06 16:40:27 GMT 2020) -----
HST Phase I Proposal 127 successfully submitted.
Receipt: # 127-2
----- Attempting Submission 3 (Fri Mar 06 16:46:16 GMT 2020) -----
FLASH level may be too high for this exposure or a long subexposure. See extended explanation in the diagnostic browser
This is a resubmission for one failed visit of SN2005IP, duplicated as new visit 55 as suggested.
-2108954146
----- Attempting Submission 1 (Mon Jun 22 21:01:30 GMT 2020) -----
----- Attempting Submission 2 (Sun Sep 27 07:44:42 GMT 2020) -----
----- Attempting Submission 3 (Tue Feb 01 20:00:13 GMT 2022) -----
We've lowered FLASH values as our Contact Scientist suggested, though the values is still higher than the warning level. But that's a known warning, and we've been told that's OK.
A Snapshot Survey of the Sites of Recent, Nearby Supernovae
During the past two decades, robotic (or highly automated) searches for supernovae (SNe) have found several thousand SNe, many of them in quite nearby galaxies (d < 30 Mpc). Most of the objects were discovered before maximum brightness, and have follow-up photometry and spectroscopy; they include some of the best-studied SNe to date. We propose to obtain HST snapshot images of the sites of some of these nearby objects, to obtain late-time photometry (through two filters) that will help reveal the origin of their lingering energy. We will also search for possible stellar remnants of Type Iax SNe, an intriguing new possibility. Moreover, the images will provide high-resolution information on the local environments of SNe that are far superior to what we can procure from the ground. For example, we will obtain color-magnitude diagrams of stars at these SN sites (those of core-collapse SNe often being especially rich in massive, luminous stars), to constrain the reddening and SN progenitor masses. We will search for light echoes around SNe, an important clue to their progenitor systems. When the SN is detected at late times (thereby providing a precise position) and deep HST archival pre-explosion images of the SN site are available, we will search for and characterize the nature of the progenitor. We will also image some "SN impostors" to verify whether they are indeed superoutbursts of luminous blue variable stars and survived the explosions, or a new/weak class of massive-star explosions. Our proposed snapshots in Cycle 28 will complement and extend the set of existing SN sites imaged with HST by various investigators in previous cycles.
We wish to obtain WFC3 images of the sites of nearby, recent SNe discovered or monitored by LOSS. Most of the objects are core-collapse SNe, which have massive, short-lived progenitors (making it also possible to study individual stars in their local environment), but several SNe Ia will also be imaged to obtain late-time measurements in crowded environments and provide statistics on light echoes. The use of standard wide bands will permit direct comparisons with other HST observations. Although there are tradeoffs, we feel that WFC3 is superior to ACS for our purposes, due to its higher resolution and, more importantly, shorter overhead time for the relatively brief snapshot visits. Note that a substantial part of the host galaxies of the SNe will be imaged with WFC3, and the data can be used for many other studies, such as galaxy morphology, stellar populations, variable stars, star clusters, H II regions, and the search for future SN progenitors. We will adjust the pointing coordinates of the telescope to make sure the SN sites and the maximum portion of their host galaxies are imaged.
Accurate astrometry will generally be needed in order to locate the faint SN in its environment. This requires imposing an independent reference grid onto the WFC3 image, using stars that have been measured in deep, ground-based images and tied to the USNO B1 systems. We have access to telescopes at the Lick, Palomar, CFHT, Gemini, Magellan, and Keck Observatories, where we have been obtaining such images of each SN field. We have verified in previous studies that the number of stars typically visible in the HST and ground-based images is sufficient for our purposes.
Given our desire to go fairly deep, and the advantage of having some color information for SNe (and their environments), the use of at least two filters is deemed necessary, and we choose F555W (V ) and F814W (I) filters for our proposed visits. The F814W filter is sensitive to massive, evolved stars in the neighborhood of core-collapse SNe, and provides constraints on the possible circumstellar material interaction and dust formation around SNe, while the F555W filter provides color information for the SNe and the stellar content of the environment, and is also more sensitive to possible light echoes. The CR-SPLIT exposures will be dithered, as requested (Call for Proposals, Sec. 4.1.7), to improve data quality. As in previous cycles, we have substituted a number of other WFC3-UVIS broadband filters in the cases of a subset of targets to provide improved measurements tailored for each object, or to provide continuity with early time ground-based photometry.
For a single visit to be ~35 minutes long (the peak of the distribution of snapshot visits has historically been around 30-35 minutes, according to the HST Snapshot document at http://www.stsci.edu/hst/HST overview/documents/), there can be only one filter change and only one CR-SPLIT pair of WFC3 exposures through each filter. Due to a severe overhead of 5.8 min for any short (< 339 s) exposures among the first three exposures in a visit, we design a visit with the first pair of exposures having 390 s integration each, while the second pair of exposures have 390 s and 320 s integrations (the last short exposure does not impose the 5.8 min overhead penalty). This yields a total visit time of 2380 s = 37.66 minutes.
We have verified with existing HST data that uneven integration times (by a factor of 2) in a dithered CR-SPLIT exposure do not pose problems for cosmic-ray removal. The long pair of exposures (totalling 680 s) is used for the F814W filter because it has less sensitivity than the F555W filter. We have chosen 54 nearby SNe/SN impostors as the superset of targets for our snapshot study. We concentrate on the most recent ones (which have the highest probability of being detected in the HST images), as well as on long-lived SNe (as judged from their continually updated ground-based light curves).
Our total request is 54 snapshots in 54 visits (at about 37 minutes per visit). Each visit will target one SN with the F555W and F814W filters (or additional broadband WFC3 UVIS filters).
Reduced gyro operations will not significantly impact this program. The snapshot visits are only a single orbit, with several exposures during each visit. Targets either will or will not be available during particular
times, but that's always the case with Snapshot programs. The orientation of the field is not relevant, nor is the spatial scan speed.
PI Alex Filippenko led the highly successful Lick Observatory Supernova Search for more than 2 decades, has been studying images and spectra of supernovae (SNe) for more than 3 decades, and has led numerous HST studies of nearby SNe (including HST snapshot surveys similar to the one proposed here). Schuyler Van Dyk is an expert in HST photometry of SNe, in the identification of SN progenitors and determination of their masses, and in the study of stellar populations around SNe (color-magnitude diagrams, etc.). Pat Kelly has long studied the properties of host galaxies of SNe. Nathan Smith is an expert in the properties and evolution of massive stars, winds from such stars, and their environments. Ori Fox is an expert in SN late-time shock interaction and will interpret late-time detections of the targets; he also studies dust, its formation in SN ejecta, and how it affects SN photometry, spectra, and interpretations. Tom Brink has much experience obtaining and reducing ground-based spectra, and complementary data of this type will be obtained for the program. WeiKang Zheng is an expert at CCD imaging and photometry of SNe, both ground-based and HST; he conducts cosmic-ray removal, combining different images in the same filter, point-spread-function fitting, DOLPHOT photometry, etc. Thomas de Jaeger studies the light curves and spectra of Type II SNe and will combine his complementary data with the HST snapshot images. Sergiy Vasylev is a graduate student who will work on the data (under Filippenko's supervision) as part of his PhD thesis. The above investigators have fruitfully worked together in the past and have many joint HST papers. Overall, members of the team have published more than 100 papers based at least in part on HST data. They have previously conducted HST studies of SNe, both snapshot surveys and normal GO (and archival) programs.
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:visit-id "53"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 1978
:al-overhead-at-end 126
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3486
:pcs-gap 0
)
true
1
0
The scheduling data was generated by CASM 28.2.
CASM was run in Phase II mode.
(Tic-Visit
:proposal-id 16179
:visit-id "54"
:proposal-version -1
:trans-version "20200619"
:date "26-Sep-2020 06:13:14.0"
:trans-errors '(:WARNINGS 0 :ERRORS 0 :HEALTH-AND-SAFETY 0
:FATAL-ERRORS 0 :CONTINUABLE-FATALS 0)
:number-of-orbits 1
:saa-model "29"
:si-bright-earth-limb-angle 20.0
:data-volume 1154992
:tdrss-contact-duration 0
:coron NIL
)
(Tic-Obset
:proposal-id 16179
:visit-id "54"
:obset-id "54"
:pcs-mode "FGS"
)
(Tic-Orbit
:proposal-id 16179
:visit-id "54"
:orbit-number 1
:pcs-time 383
:si-vis-utilization 1936
:al-overhead-at-end 123
:internal-dur-at-end 668
:dark-offset NIL
:dark-utilization 0
:max-dark-utilization 1920
:low-sky "N"
:pcs-visibility 3149
:pcs-gap 0
)
true
1
0