Erratum:
“
AT2018cow: A Luminous Millimeter Transient
”
(
2019, ApJ, 871, 73
)
Anna Y. Q. Ho
1
, E. Sterl Phinney
2
, Vikram Ravi
1
,
3
, S. R. Kulkarni
1
, Glen Petitpas
3
, Bjorn Emonts
4
, V. Bhalerao
5
,
Ray Blundell
3
, S. Bradley Cenko
6
,
7
, Dougal Dobie
8
,
9
, Ryan Howie
3
, Nikita Kamraj
1
, Mansi M. Kasliwal
1
,
Tara Murphy
8
, Daniel A. Perley
10
, T. K. Sridharan
3
, and Ilsang Yoon
4
1
Cahill Center for Astrophysics, California Institute of Technology, MC 249-17, 1200 E California Boulevard, Pasadena, CA 91125, USA
2
Theoretical Astrophysics, MC 350-17, California Institute of Technology, Pasadena, CA 91125, USA
3
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA
4
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
5
Department of Physics, Indian Institute of Technology Bombay, Mumbai 400076, India
6
Astrophysics Science Division, NASA Goddard Space Flight Center, Mail Code 661, Greenbelt, MD 20771, USA
7
Joint Space-Science Institute, University of Maryland, College Park, MD 20742, USA
8
Sydney Institute for Astronomy, School of Physics, University of Sydney, Sydney, New South Wales 2006, Australia
9
ATNF, CSIRO Astronomy and Space Science, PO Box 76, Epping, New South Wales 1710, Australia
10
Astrophysics Research Institute, Liverpool John Moores University, IC2, Liverpool Science Park, 146 Brownlow Hill, Liverpool L3 5RF, UK
Received 2022 July 20; published 2022 August 16
In the published article Equation
(
23
)
has two typos, one in the normalization constant and one in an exponent. The corrected
version of the equation should read
⎜⎟
⎜⎟⎜⎟
⎜⎟⎜⎟
⎛
⎝
⎞
⎠
⎛
⎝
⎞
⎠
⎛
⎝
⎞
⎠
⎛
⎝
⎞
⎠
⎛
⎝
⎞
⎠
⎛
⎝
⎞
⎠
⎛
⎝
⎞
⎠
()
()
M
vM
f
Lt
1000 km s
10
yr
0.00005
1
0.5
10 erg s Hz
5 GHz 1 days
.23
wB
e
B
ppp
1
41
819
819
26
1
1
419
2
2
n
=
́
-
--
-
-
--
-
The error is re
fl
ected in the positions of the lines of constant mass-loss rate in Figure
5
. The corrected version of the
fi
gure is shown
below.
The errors did not propagate into other equations or calculations made in the text.
A.Y.Q.H. would like to thank Lindsay DeMarchi, Raffaella Margutti, and Yuhan Yao for pointing out the errors listed above.
The Astrophysical Journal,
935:62
(
2pp
)
, 2022 August 10
https:
//
doi.org
/
10.3847
/
1538-4357
/
ac847b
© 2022. The Author
(
s
)
. Published by the American Astronomical Society.
Original content from this work may be used under the terms
of the
Creative Commons Attribution 4.0 licence
. Any further
distribution of this work must maintain attribution to the author
(
s
)
and the title
of the work, journal citation and DOI.
1
ORCID iDs
Anna Y. Q. Ho
https:
/
/
orcid.org
/
0000-0002-9017-3567
E. Sterl Phinney
https:
/
/
orcid.org
/
0000-0002-9656-4032
Vikram Ravi
https:
/
/
orcid.org
/
0000-0002-7252-5485
S. R. Kulkarni
https:
/
/
orcid.org
/
0000-0001-5390-8563
Bjorn Emonts
https:
/
/
orcid.org
/
0000-0003-2983-815X
V. Bhalerao
https:
/
/
orcid.org
/
0000-0002-6112-7609
S. Bradley Cenko
https:
/
/
orcid.org
/
0000-0003-1673-970X
Dougal Dobie
https:
/
/
orcid.org
/
0000-0003-0699-7019
Nikita Kamraj
https:
/
/
orcid.org
/
0000-0002-3233-2451
Mansi M. Kasliwal
https:
/
/
orcid.org
/
0000-0002-5619-4938
Tara Murphy
https:
/
/
orcid.org
/
0000-0002-2686-438X
Daniel A. Perley
https:
/
/
orcid.org
/
0000-0001-8472-1996
Ilsang Yoon
https:
/
/
orcid.org
/
0000-0001-9163-0064
References
Chevalier, R. A. 1984, NYASA,
422, 215
Chevalier, R. A. 1998,
ApJ
,
499, 810
Ho, A. Y. Q., Phinney, E. S., Ravi, V., et al. 2019,
ApJ
,
871, 73
Margutti, R., Metzger, B. D., Chornock, R., et al. 2019,
ApJ
,
872, 18
Soderberg, A. M., Chakraborti, S., Pignata, G., et al. 2010,
Natur
,
463, 513
Figure 5.
The peak luminosity of AT2018cow on two different epochs, compared to classes of energetic transients
(
see Chevalier
1998
; Soderberg et al.
2010
)
. The
value at
Δ
t
=
22 days comes from our work. The value at
Δ
t
=
91 days comes from Margutti et al.
(
2019
)
and shows that the velocity has not slowed signi
fi
cantly.
For other sources, we choose values of peak frequency and peak luminosity as described in Appendix C of Ho et al.
(
2019
)
. AT2018cow is unusual in having a large
radio luminosity as well as a high
ν
a
, and we discuss the physical interpretation of both of these characteristics in the text. Lines of constant mass-loss rate
(
scaled to
wind velocity
)
are shown in units of 10
−
4
M
e
yr
−
1
/
1000 km s
−
1
. Note that the dotted lines assume that the radio peak is due to synchrotron self-absorption rather than
free
–
free absorption
(
FFA
)
, but that FFA has been the preferred
fi
t in some cases, such as for SN 1979C and SN 1980K
(
Chevalier
1984
)
.
2
The Astrophysical Journal,
935:62
(
2pp
)
, 2022 August 10
Ho et al.