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The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries

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The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries. / See Change.
In: The Astrophysical Journal, Vol. 912, No. 2, 87, 07.05.2021.

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See Change. The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries. The Astrophysical Journal. 2021 May 7;912(2):87. doi: 10.3847/1538-4357/abed4d

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See Change. / The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries. In: The Astrophysical Journal. 2021 ; Vol. 912, No. 2.

Bibtex

@article{3924a21a3c7945f7ba8c0bba4f1731d5,
title = "The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries",
abstract = "The See Change survey was designed to make $z>1$ cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope spanning the redshift range $z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at $z\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this proved to be a highly efficient use of HST for SN observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star-formation rates. We find that the resulting number of SNe Ia per orbit is a factor of $\sim 8$ higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel features include fully blinded SN searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 magnitudes of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host-galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper.",
keywords = "Astrophysics - Cosmology and Nongalactic Astrophysics",
author = "{See Change} and Brian Hayden and David Rubin and Kyle Boone and Greg Aldering and Jakob Nordin and Mark Brodwin and Susana Deustua and Sam Dixon and Parker Fagrelius and Andy Fruchter and Peter Eisenhardt and Anthony Gonzalez and Ravi Gupta and Isobel Hook and Chris Lidman and Kyle Luther and Adam Muzzin and Zachary Raha and Pilar Ruiz-Lapuente and Clare Saunders and Caroline Sofiatti and Adam Stanford and Nao Suzuki and Tracy Webb and Williams, {Steven C.} and Gillian Wilson and Mike Yen and Rahman Amanullah and Kyle Barbary and Hans Bohringer and Greta Chappell and Carlos Cunha and Miles Currie and Rene Fassbender and Michael Gladders and Ariel Goobar and Hendrik Hildenrandt and Henk Hoekstra and Xiaosheng Huang and Dragan Huterer and Jee, {M. James} and Alex Kim and Marek Kowalski and Eric Linder and Meyers, {Joshua E.} and Reynald Pain and Saul Perlmutter and Johan Richard and Piero Rosati and Eduardo Rozo",
note = "This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.3847/1538-4357/abed4d",
year = "2021",
month = may,
day = "7",
doi = "10.3847/1538-4357/abed4d",
language = "English",
volume = "912",
journal = "The Astrophysical Journal",
issn = "0004-637X",
publisher = "Institute of Physics Publishing",
number = "2",

}

RIS

TY - JOUR

T1 - The HST See Change Program: I. Survey Design, Pipeline, and Supernova Discoveries

AU - See Change

AU - Hayden, Brian

AU - Rubin, David

AU - Boone, Kyle

AU - Aldering, Greg

AU - Nordin, Jakob

AU - Brodwin, Mark

AU - Deustua, Susana

AU - Dixon, Sam

AU - Fagrelius, Parker

AU - Fruchter, Andy

AU - Eisenhardt, Peter

AU - Gonzalez, Anthony

AU - Gupta, Ravi

AU - Hook, Isobel

AU - Lidman, Chris

AU - Luther, Kyle

AU - Muzzin, Adam

AU - Raha, Zachary

AU - Ruiz-Lapuente, Pilar

AU - Saunders, Clare

AU - Sofiatti, Caroline

AU - Stanford, Adam

AU - Suzuki, Nao

AU - Webb, Tracy

AU - Williams, Steven C.

AU - Wilson, Gillian

AU - Yen, Mike

AU - Amanullah, Rahman

AU - Barbary, Kyle

AU - Bohringer, Hans

AU - Chappell, Greta

AU - Cunha, Carlos

AU - Currie, Miles

AU - Fassbender, Rene

AU - Gladders, Michael

AU - Goobar, Ariel

AU - Hildenrandt, Hendrik

AU - Hoekstra, Henk

AU - Huang, Xiaosheng

AU - Huterer, Dragan

AU - Jee, M. James

AU - Kim, Alex

AU - Kowalski, Marek

AU - Linder, Eric

AU - Meyers, Joshua E.

AU - Pain, Reynald

AU - Perlmutter, Saul

AU - Richard, Johan

AU - Rosati, Piero

AU - Rozo, Eduardo

N1 - This is an author-created, un-copyedited version of an article accepted for publication/published in The Astrophysical Journal. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at doi:10.3847/1538-4357/abed4d

PY - 2021/5/7

Y1 - 2021/5/7

N2 - The See Change survey was designed to make $z>1$ cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope spanning the redshift range $z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at $z\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this proved to be a highly efficient use of HST for SN observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star-formation rates. We find that the resulting number of SNe Ia per orbit is a factor of $\sim 8$ higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel features include fully blinded SN searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 magnitudes of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host-galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper.

AB - The See Change survey was designed to make $z>1$ cosmological measurements by efficiently discovering high-redshift Type Ia supernovae (SNe Ia) and improving cluster mass measurements through weak lensing. This survey observed twelve galaxy clusters with the Hubble Space Telescope spanning the redshift range $z=1.13$ to $1.75$, discovering 57 likely transients and 27 likely SNe Ia at $z\sim 0.8-2.3$. As in similar previous surveys (Dawson et al. 2009), this proved to be a highly efficient use of HST for SN observations; the See Change survey additionally tested the feasibility of maintaining, or further increasing, the efficiency at yet higher redshifts, where we have less detailed information on the expected cluster masses and star-formation rates. We find that the resulting number of SNe Ia per orbit is a factor of $\sim 8$ higher than for a field search, and 45% of our orbits contained an active SN Ia within 22 rest-frame days of peak, with one of the clusters by itself yielding 6 of the SNe Ia. We present the survey design, pipeline, and SN discoveries. Novel features include fully blinded SN searches, the first random forest candidate classifier for undersampled IR data (with a 50% detection threshold within 0.05 magnitudes of human searchers), real-time forward-modeling photometry of candidates, and semi-automated photometric classifications and follow-up forecasts. We also describe the spectroscopic follow-up, instrumental in measuring host-galaxy redshifts. The cosmology analysis of our sample will be presented in a companion paper.

KW - Astrophysics - Cosmology and Nongalactic Astrophysics

U2 - 10.3847/1538-4357/abed4d

DO - 10.3847/1538-4357/abed4d

M3 - Journal article

VL - 912

JO - The Astrophysical Journal

JF - The Astrophysical Journal

SN - 0004-637X

IS - 2

M1 - 87

ER -