Date and Time of the Query: 2019-06-19 T07:49:32 PDT
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Notes for object Sextans B

13 note(s) found in NED.

1. 2009AJ....138.1203M
Re:DDO 070
A.7. DDO 70 is a small galaxy (47 useable regions) at a moderate distance
(1.3 Mpc). It has had steady, slow star formation over the last 200 Myr, with
peak masses of only ~8 * 10^3^ M_sun_. Like DDO 75, DDO 70 has formed only a
few clusters over the past 10 Myr and only a few clusters before 200 Myr ago.
There are no star-forming regions found beyond R_H{alpha}_, and so no comparison
can be made between the galaxy interior and exterior to R_H{alpha}_. A plot of
age versus mass is presented in Figure 3 with regions color coded according to
the inner 50% and the outer 50% of regions.

2. 2008MNRAS.388..500E
Re:UGC 05373
UGC 5373 (Sextans B, KIG 388). This dwarf galaxy is part of the Local Group. Our
H{alpha} map is in good agreement with the H{alpha} maps from Hunter & Elmegreen
(2004) and James et al. (2004). The H{alpha} velocity field presents a low
amplitude velocity gradient (~30 km s^-1^) barely visible in the
position-velocity diagram. Both major-axis orientation and inclination are
difficult to determine; nevertheless, the kinematical major-axis seems to be
quite different (~30^deg^) from the photometric major-axis probably due to
non-circular motions. The H{alpha} rotation curve is ill-defined in the central
part, with a possible counter-rotation within 15 arcsec from the centre, but
rises rapidly beyond 30 arcsec and seems to reach a plateau at about 50 arcsec,
in agreement with the H I data from Hoffman et al. (1996) who miss the rising
part because of their poor resolution (and possibly lack of H I at the centre).
We also agree that this galaxy is almost face-on (from the kinematics we find
10^deg^, with an uncertainty of 18^deg^ and (Hoffman et al. 1996) find 18^deg^),
whereas the photometry suggests 60^deg^ (HyperLeda). However, our very low
inclination value may lead us to overestimate the rotation velocities.

3. 2004ApJ...608...42S
Re:Sextans B
Sextans B. Sandage & Carlson (1984) discovered seven Cepheids in this
galaxy. Three of these were confirmed by Piotto et al. (1994) with
ground-based BVRI data. The same authors discovered four shorter period
Cepheids and used the entire sample to calculate a distance modulus of
25.63+-0.21 mag. Unfortunately, VI magnitudes are measured for only
three Cepheids, one with a period shorter than 8 days. The distances
listed in columns (3) and (4) of Table 3 are therefore based on only two
Cepheids, for which we adopt the data from Piotto et al. (1994).

4. 2003A&A...411..391L
Re:KIG 0388
CIG 388 - This is a Local Group member (Sextans B).

5. 2002A&A...389..812K
Re:Sextans B
Sextans B. According to Sakai et al. (1997) the distance to
this dIrr galaxy found from the luminosity of its RGB stars
is 1.29 +/- 0.07 Mpc. Our estimate of its distance,
1.36 +/- 0.07 Mpc, agrees well with the previous one.

6. 1997AstL...23..656G
Re:Sextans B
Sextans B. We constructed the LF from the color-magnitude diagram of Hoessel
(1986). The CCD photometry of Tosi et al. (1991) does not cover the entire
galaxy. However, by assuming that the data on region A correspond to half of
the galaxy and by multiplying the values of the LF that corresponds to region A
by 2, the estimate of V(5) is confirmed. After their reduction to the CCD scale
of Tosi et al. (1991) (by subtracting 0.2^m^), the photographic data of Sandage
and Carlson (1985a) confirm the estimate of V(5). In Georgiev et al. (1997b)
and Karachentsev and Tikhonov (1994), this galaxy greatly deviates from the
calibration relations of the brightest-star method. Referring to the
reliability of its Cepheid distance modulus (Piotto et al. 1992b), we may
conclude that it is a less clear representative of the intermediate type of
irregular spheroidal dwarf galaxies; Phoenix and Pisces are good examples of
such galaxies.

7. 1994CAG1..B...0000S
Re:Sextans B
Jan 7/8, 1976
103aO + GG13
30 min
Sextans B, at the same distance as Sextans
A based on a study of Cepheids in both galaxies
(Sandage and Carlson 1985), has a redshift
corrected to the centroid of the Local Group of
v_o = +114 km/s. The Cepheid distance modulus is
m - M = 26.2. Hence, in the direction of Sextans A
and B the zero-velocity surface of the Local
Group is closer to the Sun than 1.7 Mpc.
The brightest blue stars begin to resolve at
B = 19; the brightest red supergiants begin to
resolve at about V = 19.

8. 1994AJ....107.1328v
Re:Sextans B
Sextans B = DDO 70
The distance to this dwarf irregular has been discussed by Tosi et al.
(1991), who conclude that (m - M)_0_ = 25.6, corresponding to D = 1.3 Mpc.
This is slightly smaller than the value D = 1.7 Mpc that Sandage &
Garlson (1985) obtained from photographic observations of Cepheids. These
authors also suggest that Sex A and Sex B, which have similar distances
and are separated by only 10.4^deg^ on the sky, may form a physical pair.
The position of Sex B in the V__sun_ versus cos{theta} plot suggests
that this dwarf irregular may be located just beyond the zero velocity
surface of the local Group.

9. 1976RC2...C...0000d
Re:[RC2] A0957+05
= DDO 070
Dwarf Sextans B system.
HII Regions:
Ap. J. Suppl., 27, No. 239, 1974.

10. 1973UGC...C...0000N
Re:UGC 05373
DDO 70, A0957 in RC1

11. 1973AISAO...8....3K
Re:KIG 0388
Sextans B

12. 1966AJ.....71..922v
Re:DDO 070
= Sextans B
Possible member of Local Group.

13. 1964RC1...C...0000d
Re:[RC1] A0957
= Sextans B
See F. Zwicky, Morphological Astronomy, p. 225, 1957.

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