Date and Time of the Query: 2019-05-25 T20:36:42 PDT
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Notes for object SN 1960F

2 note(s) found in NED.

1. 1999AJ....118.2331V
Re:SN 1960F
As is the case for SN 1988M in section 3.1.9, the environment of
the SN Ia 1960F is in the deep F555W and F814W images, taken as part of
a project to measure a Cepheid-based distance to SN 1960F (Saha et al.
1996a). Seventeen epochs of F555W imaging and four epochs of F814W
imaging were obtained, each set of images consisting of a pair of 2000 s
exposures. The method for analyzing these images was the same as for the
environment of SN 1979C (see Van Dyk et al. 1999): a model PSF was
produced, stars were located, photometry was performed with DAOPHOT and
ALLSTAR, and the results were averaged over all epochs. Faint stars that
were not found in the individual images were located in summed images,
and the resulting photometry was appended to the results for the
individual images. We performed the photometry over a large area of the
image. Although crowding was severe in some regions, the photometry with
a TinyTim PSF led to satisfactory results. The SN environment on the
summed F555W image is shown in Figure 18. We used the accurate absolute
position for the SN from Porter (1993). The SN occurred in a region
between two spiral arms in NGC 4496A.
We show in Figure 19 the CMD produced by our photometry of the
larger environment around the SN, along with the B94 isochrones,
adjusted for both the reddening (E[V-I] = 0.04) and the distance
modulus(m - M = 31.03) from Saha et al. (1996a), and transformed to
WFPC2 synthetic magnitudes. A large number of populations are revealed
in these deep images, from quite blue to very red, including hot main
sequence stars, red supergiants, and the tip of the red giant branch.
Reddening and crowding are undoubtedly affecting the observed stellar
magnitudes and colors. However, even these images are not deep enough to
see populations with ages >~500 Myr, from which SNe Ia are thought to
arise. After all resolved stars were subtracted away, we estimated a
magnitude and measured a color for the environment, through a 1.5"
aperture centered on the SN position, of m_F555W_ ~ 30.1 mag (the
magnitude of pixels 1 {sigma} above the mean background) and F555W -
F814W ~ 0.6 mag, consistent with a background of late-F stars,
presumably giants with ages >~300 Myr, or possibly fainter, reddened
early-type stars.

2. 1961PASP...73..175H
Re:SN 1960F
No. 8. Appeared 38" east and 24" north of the nucleus of the Sc galaxy NGC 4496.
Not seen on a plate taken March 20, 1960. Visible April 17 through July 18,
1960. No observations from August through December, 1960. Still visible at about
magnitude 20.0 on January 15, 1961. A member of the Virgo cluster, NGC 4496 is
the larger member of what appears to be a double galaxy. The smaller member of
the double is situated at the south-following edge of NGC 4496 and intermingled
with it. The supernova almost certainly belongs to NGC 4496 as its distance from
the companion galaxy is large.
The spectrum of the supernova has been photographed by Greenstein at the
200-inch; he classifies it as of type I.

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