DRAFT
2024-10-04 01:59:31
Type: Object/s-Data/Analysis
Bibcode: 2024TNSAN.283....1B
DAO photometric follow-up of selected transients (Oct. 2024)
Authors: D. D. Balam (Dominion Astrophysical Observatory, National Research Council of Canada) & Eric Hess (RAO/University of Calgary)
Source Group: DAO_OTS
Keywords: Photometry
Abstract:
We present (SDSS) g&r filter photometric follow up observations of selected optical transients obtained using the 1.82-m Plaskett telescope of the (Dominion Astrophysical Observatory) National Research Council of Canada during the October 2024 dark run.
SDSS filter photometry of transients
Object UT g(SDSS) g-r Presumed Host z (Published)
2024wsh 2024 10 02.231 21.11 (0.08) +0.34 (0.12) SDSS J223203.58+160520.1 0.430 p
2024wsz 2024 10 02.391 19.25 (0.02) -0.03 (0.03) WISEA J011610.03+394118.0 0.102 s
2024wtu 2024 10 02.294 17.71 (0.01) +0.22 (0.02) SDSS J232330.82+185353.9 0.036 p
2024wvi 2024 10 02.169 20.05 (0.06)   SDSS J211913.18+102514.4 0.140 p
2024wvz 2024 10 02.329 20.70 (0.04) +0.28 (0.07) SDSS J000158.05+263034.9 0.275 p
2024wxx 2024 10 02.134 19.28 (0.03) -0.20 (0.06) WISEA J205644.12+283707.7  
2024wyx 2024 10 02.454 20.15 (0.06) +0.64 (0.07) SDSS J021410.42+231218.0 0.219 p

Photometric observations obtained with the 1.82-m Plaskett telescope are differential (SDSS gri filters) and measured from stars in either the Sloan Digital Sky Survey (Skyserver) or the Pan-STARRS release 1 (PS1) Survey - DR1.

The transient host galaxy light in our photometric measurement is minimized via one of two methods: Reference images are downloaded from the PanSTARRS image access (Flewelling, H. A., et al.) and are convolved, using the nightly PSF to match our images. The reference is then subtracted from our co-added images. A secondary photometric standard is defined and retained on the subtracted image using a pixel mask. 

A second method involves creating a model galaxy, using the IRAF artdata packages, scaling it to the images and subtracting the host galaxy. The differential photometry  was then performed using Image Reduction and Analysis Facility (IRAF) (Tody, D. 1986, "The IRAF Data Reduction and Analysis System").

Note:  photometric redshifts are marked 'p' and spectroscopic redshifts are marked 's'. All host redshifts are via the SDSS Skyserver.

Show current TNS values
Catalog Name Reported RA Reported DEC Reported Obj-Type Reported Redshift Host Name Host Redshift Remarks TNS RA TNS DEC TNS Obj-Type TNS Redshift
TNS 2024wsh 22:32:03.521 +16:05:19.83 22:32:03.521 +16:05:19.83
TNS 2024wsz 01:16:09.907 +39:41:10.28 01:16:09.901 +39:41:10.36
TNS 2024wtu 23:23:30.591 +18:53:55.71 SN II 0.02 23:23:30.586 +18:53:55.57 SN II 0.02
TNS 2024wvi 21:19:13.306 +10:25:14.39 21:19:13.309 +10:25:14.37
TNS 2024wvz 00:01:58.127 +26:30:34.84 00:01:58.129 +26:30:34.91
TNS 2024wxx 20:56:44.230 +28:37:17.70 20:56:44.230 +28:37:17.70
TNS 2024wyx 02:14:10.502 +23:12:18.02 02:14:10.502 +23:12:18.02

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