DRAFT
2024-09-11 03:44:42
Type: Announcement-Data Release
Bibcode: 2024TNSAN.249....1B
DAO photometric follow-up of selected transients
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 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
SDSS filter photometry of transients
Object UT g (SDSS) g-r Presumed host z (published)
2024szl 2024 08 29.324 19.81 (0.03) +0.21 (0.10) SDSS J223332.11+115630.0 0.011 p
2024szx 2024 08 29.276 19.24 (0.02) +0.52 (0.04)    
2024tdd 2024 08 29.420 19.96 (0.03)      
2024tta 2024 08 29.17 19.71 (0.03) +0.26 (0.04) SDSS J172004.97+445524.3 0.357 p
2024tuf 2024 08 29.228 18.42 (0.02) +0.29 (0.02) WISEA J220832.40+400142.6  
2024tuk 2024 08 30.361 18.82 (0.02) +0.73 (0.03) WISEA J205658.84+670046.6 0.029 s
2024twg 2024 08 30.424 19.10 (0.02) +0.68 (0.03) WISEA J005553.84+473046.0 0.723 d
2024uzy 2024 09 09.229 18.97 (0.02) +0.11 (0.03) SDSS J220045.09+230325.5 0.118 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 2024szl 22:33:32.463 +11:56:28.68 22:33:32.463 +11:56:28.68
TNS 2024szx 22:25:25.417 +15:57:36.93 22:25:25.417 +15:57:36.93
TNS 2024tdd 00:50:12.252 +42:24:43.17 00:50:12.252 +42:24:43.17
TNS 2024tta 17:20:05.082 +44:55:24.22 17:20:05.082 +44:55:24.22
TNS 2024tuf 22:08:32.194 +40:01:45.23 22:08:32.131 +40:01:44.49
TNS 2024tuk 20:56:57.785 +67:00:40.02 20:56:57.785 +67:00:40.02
TNS 2024twg 00:55:53.444 +47:30:51.33 00:55:53.444 +47:30:51.33
TNS 2024uzy 22:00:45.190 +23:03:24.59 22:00:45.186 +23:03:24.67 SN Ia 0.0868

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