CaltechAUTHORS
  A Caltech Library Service

Two New Calcium-rich Gap Transients in Group and Cluster Environments

Lunnan, R. and Kasliwal, M. M. and Cao, Y. and Hangard, L. and Yaron, O. and Parrent, J. T. and McCully, C. and Gal-Yam, A. and Mulchaey, J. S. and Ben-Ami, S. and Filippenko, A. V. and Fremling, C. and Fruchter, A. S. and Howell, D. A. and Koda, J. and Kupfer, T. and Kulkarni, S. R. and Laher, R. and Masci, F. and Nugent, P. E. and Ofek, E. O. and Yagi, M. and Yan, Lin (2017) Two New Calcium-rich Gap Transients in Group and Cluster Environments. Astrophysical Journal, 836 (1). Art. No. 60. ISSN 0004-637X. https://resolver.caltech.edu/CaltechAUTHORS:20170214-095909820

[img] PDF - Published Version
See Usage Policy.

3838Kb
[img] PDF - Submitted Version
See Usage Policy.

4Mb

Use this Persistent URL to link to this item: https://resolver.caltech.edu/CaltechAUTHORS:20170214-095909820

Abstract

We present the Palomar Transient Factory discoveries and the photometric and spectroscopic observations of PTF11kmb and PTF12bho. We show that both transients have properties consistent with the class of calcium-rich gap transients, specifically lower peak luminosities and rapid evolution compared to ordinary supernovae, and a nebular spectrum dominated by [Ca II] emission. A striking feature of both transients is their host environments: PTF12bho is an intracluster transient in the Coma Cluster, while PTF11kmb is located in a loose galaxy group, at a physical offset ~150 kpc from the most likely host galaxy. Deep Subaru imaging of PTF12bho rules out an underlying host system to a limit of M_R > -8.0 mag, while Hubble Space Telescope imaging of PTF11kmb reveals a marginal counterpart that, if real, could be either a background galaxy or a globular cluster. We show that the offset distribution of Ca-rich gap transients is significantly more extreme than that seen for SNe Ia or even short-hard gamma-ray bursts (sGRBs). Thus, if the offsets are caused by a kick, they require higher kick velocities and/or longer merger times than sGRBs. We also show that almost all Ca-rich transients found to date are in group and cluster environments with elliptical host galaxies, indicating a very old progenitor population; the remote locations could partially be explained by these environments having the largest fraction of stars in the intragroup/intracluster light following galaxy–galaxy interactions.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://doi.org//10.3847/1538-4357/836/1/60DOIArticle
http://iopscience.iop.org/article/10.3847/1538-4357/836/1/60/metaPublisherArticle
https://arxiv.org/abs/1612.00454arXivDiscussion Paper
ORCID:
AuthorORCID
Lunnan, R.0000-0001-9454-4639
Kasliwal, M. M.0000-0002-5619-4938
Cao, Y.0000-0002-8036-8491
Yaron, O.0000-0002-0301-8017
McCully, C.0000-0001-5807-7893
Gal-Yam, A.0000-0002-3653-5598
Ben-Ami, S.0000-0001-6760-3074
Filippenko, A. V.0000-0003-3460-0103
Fremling, C.0000-0002-4223-103X
Howell, D. A.0000-0003-4253-656X
Koda, J.0000-0002-8762-7863
Kupfer, T.0000-0002-6540-1484
Kulkarni, S. R.0000-0001-5390-8563
Laher, R.0000-0003-2451-5482
Masci, F.0000-0002-8532-9395
Nugent, P. E.0000-0002-3389-0586
Ofek, E. O.0000-0002-6786-8774
Yan, Lin0000-0003-1710-9339
Additional Information:© 2017 The American Astronomical Society. Received 2016 November 23; revised 2016 December 20; accepted 2016 December 21; published 2017 February 8. R.L. thanks Andrew Wetzler, Wen-fai Fong, Mark Sullivan, Dan Milisavljevic, Giorgos Leloudas, Jesper Sollerman, and Ryan Chornock for useful discussions and acknowledges helpful interactions with Lars Bildsten, Eliot Quataert, and Dan Kasen at a PTF Theory Network retreat funded by the Gordon and Betty Moore Foundation through Grant GBMF5076. We thank J. Silverman, B. Dilday, J. Bloom, B. Sesar, D. Levitan, P. Groot, D. Perley, A. Horesh, K. Mooley, and D. Xu for assisting with the observations presented in this paper. The Intermediate Palomar Transient Factory project is a scientific collaboration among the California Institute of Technology, Los Alamos National Laboratory, the University of Wisconsin–Milwaukee, the Oskar Klein Center, the Weizmann Institute of Science, the TANGO Program of the University System of Taiwan, and the Kavli Institute for the Physics and Mathematics of the Universe. Support for HST Program GO-13864 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the AURA, Inc., under NASA contract NAS 5-26555. We thank F. Yuan, M. Sullivan, D. Perley, R. M. Quimby, and S. B. Cenko for their contributions to the HST proposal. This work was supported by the GROWTH project funded by the National Science Foundation under Grant 1545949. The National Energy Research Scientific Computing Center, which is supported by the Office of Science of the U.S. Department of Energy under Contract No. DE-AC02-05CH11231, provided staff, computational resources, and data storage for this project. A.G.-Y. is supported by the EU/FP7 via ERC grant No. 307260, the Quantum Universe I-Core program by the Israeli Committee for planning and funding, and the ISF, Minerva and ISF grants, WIS-UK "making connections," and Kimmel and YeS awards. A.V.F. is grateful for financial support from the Christopher R. Redlich Fund, the TABASGO Foundation, and NSF grant AST-1211916. D.A.H. and C.M. are supported by NSF grant AST-313484. This research has made use of the NASA/IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. Some of the data presented herein were obtained at the W.M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W.M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Mauna Kea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain. Facilities: PO:1.2m, PO:1.5m, PO:Hale, Keck:I, Keck:II, Subaru, HST.
Group:Infrared Processing and Analysis Center (IPAC), Palomar Transient Factory, Astronomy Department
Funders:
Funding AgencyGrant Number
Gordon and Betty Moore FoundationGBMF5076
NASANAS 5-26555
NSFOISE-1545949
Department of Energy (DOE)DE-AC02-05CH11231
European Research Council (ERC)307260
Israeli Committee for Planning and BudgetingUNSPECIFIED
Israel Science FoundationUNSPECIFIED
MINERVA (Israel)UNSPECIFIED
Weizmann-UKUNSPECIFIED
Kimmel AwardUNSPECIFIED
YeS AwardUNSPECIFIED
Christopher R. Redlich FundUNSPECIFIED
TABASGO FoundationUNSPECIFIED
NSFAST-1211916
NSFAST-313484
NASA/JPL/CaltechUNSPECIFIED
W. M. Keck FoundationUNSPECIFIED
Subject Keywords:supernovae: general – supernovae: individual (PTF11kmb, PTF12bho, PTF10hcw, SN 2005E)
Issue or Number:1
Record Number:CaltechAUTHORS:20170214-095909820
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20170214-095909820
Official Citation:R. Lunnan et al 2017 ApJ 836 60
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:74294
Collection:CaltechAUTHORS
Deposited By: Tony Diaz
Deposited On:15 Feb 2017 05:18
Last Modified:22 Nov 2019 22:42

Repository Staff Only: item control page