Szalai, Tamás

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ATel OnPatreonMastodonTwitterPost | Search | PoliciesCredential | Feeds | Email26 Sep 2023; 06:44 UTThis space for free for your conference.[ Previous | Next | ADS  ]Spitzer constraints on pre-explosion variability of theSN 2023ixf progenitorATel #16042; T. Szalai (University of Szeged, Hungary), S. Van Dyk (Caltech/IPAC,USA)on 20 May 2023; 18:41 UTCredential Certification: Tamas Szalai (szaszi@titan.physx.u-szeged.hu)Subjects: Infra-Red, Cataclysmic Variable, Star, Supernovae, TransientReferred to by ATel #: 16060, 16064TweetSupernova (SN) 2023ixf was discovered by K. Itagaki in the very nearby galaxy (d=6.4Mpc; Shappee & Stanek 2011, ApJ, 733, 124) Messier 101 (M101; NGC 5457) on05/19/2023 and has been classified as a Type II SN by Perley et al. (AstroNote 2023-119).Since M101 was a target by several programs during the Spitzer Space Telescopemission, we analyzed publicly available data in order to follow the possible pre-explosionphotometric evolution of the progenitor on the archival mid-infrared images. A single-epochdataset exists obtained during the Spitzer Cryogenic Mission (03/08/2004, program 60[GORDON_M101], PI: G. Rieke), while the SN field was serendipitously imaged manyadditional epochs between 2012 and 2019 during the Post-Cryogenic Mission (mostly partof the SPIRITS program; IDs 10136, 11063, 13053, 14089; PI M. Kasliwal). A point sourceis clearly detectable at 3.6 and 4.5 microns in Spitzer/IRAC images at the coordinates ofthe SN (RA=14:03:38.51, Dec=+54:18:42:10; Perley et al. 2023) at all epochs between2004 and 2019, while there is no detection at 5.8 and 8.0 microns obtained in 2004. Wedetermined the mid-IR fluxes of the source by applying simple aperture photometry on the3.6 and 4.5 micron Spitzer/IRAC images. While there are some fluctuations, ourpreliminary dataset -- at least, to within the uncertainties -- does not exhibit significant fluxchanges in the preceding ~20 yrs before the explosion (which, if would be detected, couldbe an indication of pre-explosion eruptive mass-loss processes, if this object is theprogenitor). Nevertheless, it is worth performing a more detailed analysis of this multi-wavelength, pre-explosion dataset of this object at a future time. It also remains for thisobject to be confirmed as the progenitor candidate via accurate astrometric registrationwith images showing the SN. If it is the progenitor candidate, based on weighted means ofour preliminary photometry, the object had a brightness at 3.6 and 4.5 microns of 17.6 and17.2 mag (+/- 0.2 mag in each), respectively. Assuming only Galactic foreground extinction(A[V]=0.024 mag; leading to negligible extinction in the IRAC bands), these correspond toabsolute brightnesses of -11.4 and -11.8 mag (+/- 0.3 mag in each). These are both higherthan what we would expect for a bare red supergiant (RSG) photosphere (approximatelyRelated16075 Fermi-LAT gamma-rayobservations of SN 2023ixf16073 Chandra X-ray detection ofsupernova SN 2023ixf in M10116067 Followup of SN2023ixf withHCT on 28th May, 2023.16065 SN 2023ixf continues to risein hard X-rays16064 Search for the progenitor ofSN 2023ixf in archivalAstroSat UVIT images16060 Search the XMM-Newtonarchival data for theprogenitor of SN 2023ixf16053 Optical spectra of SN 2023ixfwith the HCT on 22nd May2023.16052 uGMRT radio upper limit onSupernova SN 2023ixf in M10116051 X-ray emission of SN 2023ixfand its progenitor16050 Detection of candidateprogenitor of SN 2023ixf inHST archival data16049 NuSTAR detection of SN2023ixf in M10116047 Multi-Band PhotometricFollow-up of SN 2023ixf16045 Optical observations of SN2023ixf at Teide Observatory16044 MAXI/GSC upper limit of SN2023ixf in M 10116042 Spitzer constraints on pre-explosion variability of the SN2023ixf progenitor16040 New Maximum NIR flare of theFSRQ HB891420+32616021 New Giant NIR flare of theFSRQ HB891420+326-9.6 and -9.3 mag, respectively), which implies that, if this is a RSG, circumstellar dust maybe a factor. We note, for instance, that for SN 2017eaw, the progenitor had luminosities of-11.46 and -11.67 mag in the two Spitzer bands (Van Dyk et al. 2019, ApJ, 875, 136). If theSN 2023ixf progenitor were analogous to the SN 2017eaw progenitor, it may have had aninitial mass of approximately 15 solar masses. A plot of our preliminary Spitzer photometryon the progenitor candidate for SN 2023ixf can be found at the link below.http://titan.physx.u-szeged.hu/~szaszi/SN2023ixf_Spitzer_preexplosion_photometry.png[ Telegram Index ]R. E. Rutledge, Editor-in-ChiefDerek Fox, Editor

Spitzer constraints on pre-explosion variability of the SN 2023ixf progenitor

http://real.mtak.hu/174927/3/ATel%20%2316042_%20Spitzer%20constraints%20on%20pre-explosion%20variability%20of%20the%20SN%202023ixf%20progenitor.pdf

Spitzer constraints on pre-explosion variability of the SN 2023ixf progenitor

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