NASA/IPAC EXTRAGALACTIC DATABASE
Date and Time of the Query: 2019-04-24 T04:54:40 PDT
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Notes for object NGC 3073

6 note(s) found in NED.


1. 2004ApJS..151..193S
Re:NGC 3073
Tracing the wind out to such large distances strengthens the case that
the peculiar H I distribution of the dwarf galaxy NGC 3073 (10.0' away
from NGC 3079, corresponding to a minimum physical separation of 49.7
kpc) is due to a wind from NGC 3079 (Irwin et al. 1987) ram-pressure
stripping the ISM of this dwarf galaxy. If this is occurring, there
should be X-ray and H{alpha} emission associated with a bow shock
upstream from NGC 3073 (similar to the Lehnert et al. 1999 model for the
cloud found 11 kpc to the north of M82). We find no statistically
significant level of X-ray emission associated with NGC 3073 itself. The
upper limit on the soft X-ray emission within a 2' diameter aperture
centered on NGC 3073 (this extends ~1' ~ 5 kpc further upstream than the
H I) is less than 1.3 x 10^-3^ counts s^-1^ (3 {sigma}, 0.3-2.0 keV
energy band). Assuming a total absorbing column equal to the foreground
Galactic column of NH = 2 x 10^20^ cm^-2^, emission from a hot plasma with
a temperature similar to what Lehnert et al. (1999) found for the M82
northern cloud (kT {approx} 0.8 keV), and using the appropriate spectral
responses, this corresponds to a flux limit of fX < 6 x 10^-1^5 ergs s^-1^
cm^-2^, and L_X_ < 2 x 10^38^ ergs s^-1^. By way of comparison, the M82
northern cloud has a soft X-ray luminosity of 2 x 10^38^ ergs s^-1^ and
a very similar H{alpha}luminosity. Were the M82 northern cloud at a
distance of 50 kpc from M82, we might expect its X-ray and
H{alpha}luminosities to be a factor of (50/11)^2^ ~ 20 times fainter,
given that it would intercept a significantly smaller fraction of the
superwind's mechanical energy. Deep optical imaging may be a promising
way of determining whether there really is a bow shock with luminosity
L_H{alpha}_~ L_X_ ~ 10^37^ ergs s^-1^ upwind of NGC 3073 (to our
knowledge this has not been attempted, despite it being suggested by
Irwin et al. 1987).

2. 1995ApJS...98..477H
Re:NGC 3073
An H II region spectrum coupled with deep Balmer absorption lines
indicate that the stellar population of NGC 3073 is very young.
Filippenko & Sargent (1992 and references therein) postulate that the
copious star formation observed in NGC 3073 might have been triggered by
the superwind from NGC 3079 (see above), which, in projection, points in
the direction of NGC 3073.

3. 1976RC2...C...0000d
Re:NGC 3073
= MRK 0131
= Holm 156b
Pair with NGC 3079 (Holm 156a) at 10 arcmin
Photometry (10 Color):
Ap. J., 179, 731, 1973.
Spectrum: Previously reported as blue continuum with no lines
Ap. J., 173, 7, 1972.

4. 1973UGC...C...0000N
Re:UGC 05374
E pec? (de Vaucouleurs)
UGC 05387 at 9.9

5. 1964RC1...C...0000d
Re:NGC 3073
= Holm 156b
Pair with NGC 3079 (Holm 156a) at 10 arcmin.

6. 1918PLicO..13....9C
Re:NGC 3073
Very bright; fading out rapidly toward the edges; round, 0.3' in diameter,
structureless.


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