0Assigned ID: 5230
----- Attempting Submission 1 (Mon Mar 25 19:49:30 GMT 2024) -----
HST Phase I Proposal 5230 successfully submitted.
Receipt: # 5230-1
----- Attempting Submission 2 (Tue Mar 26 12:32:47 GMT 2024) -----
HST Phase I Proposal 5230 successfully submitted.
Receipt: # 5230-2
----- Attempting Submission 3 (Tue Mar 26 20:35:39 GMT 2024) -----
HST Phase I Proposal 5230 successfully submitted.
Receipt: # 5230-3
----- Attempting Submission 4 (Tue Mar 26 21:39:56 GMT 2024) -----Resubmission by Weikang on Nov 14, updating FLASH value to be 10 (from 12) for F625W and 12 (from 14) for F475W, as suggested by Contact Scientist Amanda Pagul.-372586291----- Attempting Submission 1 (Thu Aug 15 20:15:35 GMT 2024) -----
----- Attempting Submission 2 (Thu Nov 14 21:23:19 GMT 2024) -----Are All Type IIn Supernovae Terminal Explosions?There is evidence that some Type IIn supernovae, whose diverse spectra and light curves exhibit signs of interaction between the ejected material and circumstellar matter (CSM), are actually nonterminal outbursts of massive evolved stars such as luminous blue variables (LBVs); such objects are thus "SN impostors," at least until they undergo a terminal explosion. An outstanding example is SN 2009ip, which was classified as an SN IIn but three years later experienced an even larger, terminal explosion; the 2009 event was an SN impostor. In other cases of SNe IIn, it is possible that the initial outburst was an impostor, and the terminal explosion has not yet occurred. We propose to obtain deep, two-filter HST snapshot images of the sites of confirmed SNe IIn (> 9 years after outburst), in order to see whether the progenitor did indeed disappear and thus likely suffered a terminal explosion. The precise position of each of our targets will be known from post-eruption archival HST images. If instead we find an object at the site of the SN IIn, it is likely either the surviving progenitor, a companion star, or long-lived emission from the shocked CSM. The color of the star, obtained from the HST snapshot images, will provide a strong clue: LBVs are generally blue, ejecta-CSM interactors (with H-alpha emission) and RSG companions are red. The detection or nondetection of an object at the SN site will already provide fundamental information. However, to further explore the nature of any detected object, we will subsequently obtain essentially guaranteed, ground-based complementary spectra to search for medium/broad H-alpha emission characteristic of shocked CSM.We wish to obtain deep (mag 26--27) WFC3 images of the sites of relatively old
(>~ 9yr) SNe\,IIn that were previously imaged by HST after outburst but still visible
(data available in the HST archive), so that we know precisely where they are
located and thus where we should look. In ~30% of the cases, there are also
archival HST images from before the outburst, so that we know the brightness of
the progenitor (or have limits on it). Preliminary analysis suggests that a few with
sufficiently good data appear to likely be LBVs (based on their luminosity and colors);
more-detailed studies will be conducted in this program.
The new HST images will be compared with the existing HST images to look for an
object at the correct location. If no object is present, we will know that the progenitor
probably suffered a terminal explosion --- the conclusion made by most other previous
studies of massive-star SNe when an object is not detected at the precise location.
(Perhaps it survived but is enshrouded in dust, a possibility we will explore with a future
JWST proposal that would have been poorly motivated without an HST study first.) If,
instead, an object is present, it is either the surviving star, long-lived emission from the
SN shock, or a companion star or star cluster (light echoes are ruled out, being very
faint and/or resolved). The object's color (from the HST snapshot data) will shed
considerable light on these possibilities, which will be further explored with ground-based
spectra; we will look for H_alpha emission and measure its width. Future HST proposals
for multiband imaging will also be submitted, but we stress that this Cycle 32 proposal can
be considered successful (the main goals will have been achieved) even if no future JWST
or HST data are acquired.
WFC3 is superior to ACS for our purposes, owing to its higher resolution and 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 remedy the CTE efficiency
losses by using post-flash.
After registering the new images astrometrically with the archival HST images to pinpoint
the SN position, we will perform photometry on the new images using DOLPHOT v2.0
(Dolphin 2000). In most cases, there will either be a clearly detected isolated point source
corresponding to the SN, or no flux evident at the SN position. When no object is detected,
we will inject fake sources into the image adjacent to the SN position, and attempt to
recover them to estimate a robust limit on the object's flux. In unusual cases, nearby
sources such as stellar associations need to be simultaneously modeled to estimate the
object's flux.
Our top-priority desire is to go deep, in order to increase our chances of detecting a source
at the position of the SN. However, we also want to obtain a color of any detected object.
After running calculations on the WFC3 UVIS ETC, we decided to use the F475W (SDSS-g)
and F625W (SDSS-r) filters, distributing the available time equally between them. (We also
considered using only a single filter, F350LP, to go even deeper --- but the disadvantage is
that this provides no color information, and the observed magnitude strongly depends on the
object's SED.) The chosen filters are efficient and provide a commonly measured color.
For a visit to be ~45 min long (close to the peak of the distribution of snapshot visits;
http://www.stsci.edu/hst/HST_overview/documents/ uir/UIR_SNAP.pdf), there can be only
one dithered, CR-SPLIT pair of 900s WFC3 exposures through each of two filters. From the
ETC, we find that we reach S/N = 5 at limiting magnitudes of 26.6 (F475W) and 27.2 (F625W)
when normalized to Johnson V using the spectrum of SN~IIn 2010jl about 7 yr after explosion
and no extinction. (This input spectrum is representative of what we expect if the object exhibits
SN ejecta-CSM shock interaction.) Similarly, instead using a B0 V Pickels input spectrum (there
is no option for B0 I, closer to an LBV, but it should make little difference), we reach S/N = 5 at
limiting magnitudes of 27.0 (F475W) and 26.1 (F625W). Adopting a representative magnitude
of 26.6, the data will allow us to probe objects more luminous than roughly -6.0 mag at z = 0.007
(using H_0 = 71 km /s /Mpc), close to our average redshift. This is substantially fainter than typical
LBVs and yellow hypergiants -7 to -12), and it is even in the general range of supergiant stars
(-6 to -9; e.g., Humphreys & Davidson 1994; Smith et al. 2019). Thus, excluding a large amount
of extinction produced by dust, we should be able to detect the surviving star, if one exists.
Moreover, we will measure a broad-band color (approximately SDSS g-r), allowing us to distinguish
between an LBV (g-r <~ 0 mag in quiescence, but sometimes red because of dust formation) and
ejecta-CSM interaction (which typically produces strong H_alpha emission but almost no blue
continuum at late times) or an RSG ( g-r > ~1 mag).
In cases where an object is detected at the correct position, we will also obtain follow-up optical
spectra with large ground-based telescopes to which our team has private access and/or nationally
available time (through proposals). The main goal will be to search for intermediate-width (~1000
km /s) or broad H_alpha emission that would indicate that the object was a genuine SN whose
ejecta are interacting with (and shocking) CSM. Such emission can often be detected in very faint
objects (mag 25--26), since the flux density in the emission line far exceeds that in the continuum
(e.g., Shahbandeh et al 2023; Sziros et al. 2024). If such H_alpha emission is not detected but the
object is sufficiently bright for a decent spectrum to be obtained, that spectrum will allow us to classify
the object (LBV, RSG, etc.), ruling out a companion or associated star cluster.
If no object is detected, it will likely mean that the SN IIn did indeed explode; see, for example, the
cases of SN 2005gl (Gal-Yam & Leonard 2009) and 7 other SNe (Van Dyk et al. 2013, 2023).
However, there exists the possibility that it actually survived but is enshrouded in dust; the only way
to test this is to propose future near-IR and mid-IR JWST observations -- but this program is the
necessary first step.
Our request is 21 snapshots in 21 visits (~45 min/visit). We have chosen 21 nearby (mostly z <~ 0.01,
a few out to z = 0.02) SNe IIn that erupted >~ 9 yr ago, and for which HST images showing the SN in
the first few years post-SN are available (so we can measure precise positions).PI Alex Filippenko led the highly successful Lick Observatory Supernova Search for more than 2 decades, has been studying supernovae (SNe) for nearly 4 decades, and has led numerous HST studies of nearby SNe (including HST snapshot surveys similar to the one proposed here). He is among the first to identify both SN impostors (in 1989) and Type IIn SNe (in 1988). He can apply for Keck telescope time through the University of California, and has been very successful in doing so over the years. 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.); he is also one of the main researchers of SN impostors. Tom Matheson has long studied SNe of all kinds, including SNe IIn and SN impostors; he is an expert in the acquisition, reduction, and analysis of CCD spectra. Nathan Smith is an expert in the properties and evolution of massive stars, winds from such stars, and their environments. He can apply for LBT time through the University of Arizona. 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. Yi Yang is an expert on SNe and their late-time ejecta-CSM interaction. 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. Conor Ransome identified the SN IIn sample chosen here by conducting a very detailed investigation of SN IIn candidates and SN impostors listed in public databases (Transient Name Server, Open Supernova Catalog). Matt Darnley has over a decade of experience recovering and analyzing extragalactic pre- and post-explosion systems from HST and ground-based data (pioneering the technique for Local Group novae), and also using the DOLPHOT package. Stacey Habergham-Mawson has studied the environments of SNe IIn and SN impostors; she found that impostors and SNe IIn differ from other SN classes in terms of H-alpha environment and local metallicity. Tamas Szalai is an expert in mid-IR observations of the CSM surrounding core-collapse SNe (particularly SNe IIn), studying the possibility of late-time shock interaction and/or dust. Many of the above investigators have fruitfully worked together in the past and have numerous joint HST papers. Overall, members of the team have published hundreds of 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.Stellar Physics and Stellar Types0falseSUPPORTEDSTARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000STARSUPERNOVANOJ2000WFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF625WWFC3/UVISImagingNoNoF475WWFC3/UVISImagingNoNoF625WPOS-TARGDITHER0.145LINEfalsefalse246.84WFC3-UVIS-DITHER-LINE1falseThe scheduling data was generated by CASM 32.1.3.CASM was run in Phase II mode./private/var/folders/9y/257xdln55s571pvtmtdxt7wr0000gn/T/OPVisit11518257412147825247.xml(Tic-Visit
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