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Date and Time of the Query: 2019-05-26 T08:36:35 PDT
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Notes for object NGC 1036

7 note(s) found in NED.


1. 2005A&A...429..115N
Re:MRK 0370
4.4 Mkn 370 (NGC 1036, UGC 02160)
.
Compared to other BCDs, the iE-classified (LT86) BCD Mkn 370 is
relatively metal-rich (Z ~ Z_solar_/2, M_B_ = -17.1). Deep broad-band
surface photometry in the optical and high-resolution color and
H{alpha} maps were first presented in C01a,b, and a dedicated
spectrophotometric study of this BCD has recently been published in
Cairos et al. (2002).
.
Two major sources, separated by ~7" (380 pc), are located in the
central region of the galaxy. These correspond to the "double
nucleus" catalogued in Mazzarella & Boroson (1993) and are labeled a
and b in Fig. 4a, following the nomenclature of the latter authors.
As apparent from the contrast-enhanced inset in the J band image
(Fig. 4a), the elongated central region a splits into a brighter
southwestern and a fainter northeastern source, similar to what was
reported by Nordgren et al. (1995). The NIR images show several
fainter sources, roughly aligned with the major axis of region a.
.
The positions of both a and b coincide in the optical and in the NIR,
although b, which is a conspicuous source in the blue, is only weakly
detected in the NIR. The blue colors of this source (U-B = -0.79),
together with its emission line spectrum, flat continuum and the
large H{alpha} equivalent width (EW (H{alpha}) ~ 500 A; Nordgren et
al. 1995; Cairos et al. 2002) are indicative of a young stellar
population (ages <= 5 Myr) and substantial ionized gas contribution.
Knot a presents slightly redder colors (U-B = -0.60) and a high
continuum level, with absorption features that witness a substantial
underlying population of older stars.
.
The finding that knot b shows no appreciable old stellar background
in NIR images, but is dominated by nebular emission, indicates that
the double-nucleus morphology of Mkn 370 is attributable to
extranuclear SF activity in knot b.
.
The LSB population, traceable on our images out to R^*^ ~ 50",
provides about 80% of the J light. Its NIR colors (Table 3), as well
as the integrated B-J color of 2.3 mag, computed using data from
Cairos et al. (2002), are both consistent with an old stellar
population. In NIR wavelengths the LSB component shows a roughly
exponential slope, with a possible, but not significant slight
flattening for R^*^ <~ 30". The J band scale length, {alpha} = 0.64
kpc, is significantly smaller than the {alpha} ~ 1 kpc inferred from
B band data (Cairos et al. 2002). This difference is most likely due
to the multiple extranuclear H{alpha}-emitting sources, distributed
roughly along the optical major axis of Mkn 370 (Nordgren et al.
1995; Cairos et al. 2002). Similar to what is discussed for Mkn 600
(Sect. 4.7), these sources may contaminate the LSB emission at large
radii especially in optical wavelengths, artificially increasing the
scale length of the old population.

2. 2001ApJS..136..393C
Re:MRK 0370
Mrk 370. - V-I + H{alpha}. The color maps reveal strong color
variations, with a blue central starburst placed atop a redder, elliptical
envelope. In the H{alpha} image, and also in the U-B map, we can recognize
the two knots ("A" and "B" in the V-I map) previously catalogued as a
"double nucleus" by Mazzarella & Boroson (1993). The optical nucleus
(defined as the peak of the stellar distribution in the continuum image)
does not coincide with either of the knots but is displaced 7.2" to the
northwest of knot "B" (Garcia-Lorenzo et al. 2001).
These two knots appear to be connected by a faint bridgelike structure,
which is more visible in the H{alpha} frame. Smaller star-forming regions,
clearly resolved in the H{alpha} image, extend in the northeast and
southwest directions, resembling spiral arms. The star formation activity
is concentrated along the northeast-southwest direction, which does not
coincide with the major axis of the galaxies (as defined by the outer
isophotes in the broadband images; see Paper I).

3. 2001ApJS..133..321C
Re:MRK 0370
4.1.4. Mrk 370
This is included in the optical study of Markarian galaxies with
multiple nuclei (MB). It shows regular, elliptical, outer isophotes
surrounding two central emission sources, the bigger one located at the
optical center of the galaxy and the secondary knot to the southeast.

4. 1995ApJS...99..461N
Re:MRK 0370
The red continuum image (Figure 1a) shows Mrk 370 has an ellipticity of
0.26 indicating an inclination (if disk-like) of 44 degrees. Source a is
most nearly located in the optical center of the galaxy with a position
angle of its major axis offset from that of the very outer regions of the
galaxy by about 30 degrees. On the northeast edge of the galaxy, in line
with the major axis of source a, there are five to seven knots of
emission. On the opposite side of source a to the southwest is another
large knot. Source b is located to the southeast of the central source
at an almost 90 degree angle to the major axis of a. Figure 1b is the red
continuum subtracted H{alpha} image. Source a is brightest in the
southwest end and is seen to dim to the northeast. To the southwest of a,
at an almost equal distance as b, is a third object not noticeable in the
red image. At a heliocentric velocity of 750 (+/-20) km s^-1^ Mrk 370 is
10 Mpc away and a and b are separated by 200 pc. The knots to the
northwest and southeast resolve themselves into two rough spiral arms.
The spectra (Figure 10) again show strong emission lines. The velocity
difference is 40 (+/-28) km s^-1^.

5. 1976RC2...C...0000d
Re:NGC 1036
= MRK 0370
Spectrum, Spectrophotometry and HI 21cm:
Astr. Ap., 41, 61, 1975.

6. 1973UGC...C...0000N
Re:UGC 02160
S0-type object but asymmetric
Bright probably complex central region

7. 1971Afz.....7..299M
Re:MRK 0370
Elongated along Dec; a faint corona is noticed.


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