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Notes for object IC 1613

14 note(s) found in NED.

1. 2009AJ....138.1203M
Re:IC 1613
A.2. IC 1613 IC 1613 is our third nearest galaxy at 0.7 Mpc, and second most
populous galaxy with 342 useable star-forming regions. Because it is nearby, we
were able to trace the star-forming regions to masses as low as ~30 M_sun_.
The minimum mass for which we should see all currently definable star-forming
regions from the last 500 Myr is approximately 3 * 10^3^ M_sun_, as
indicated by the dashed horizontal line in Figure 3. The maximum mass formed is
of order 3 * 10^4^ M_sun_. In IC 1613, there has been more-or-less
continuous star formation over the last 1 Gyr. The apparent formation rate of
massive star-forming regions (>3 * 10^3^ M_sun_ for IC 1613) from log age of 7.0
to 8.5 is 0.03 regions Myr^-1^.
IC 1613 has an H{alpha} profile that ends before the UV star-forming regions
end. The H{alpha} only extends to a radius of 7.5" from the center of the
galaxy, and we see star-forming regions in the UV out to a radius of 9.3'.
There are far more massive regions inside R_H{alpha}_ than outside. The clusters
beyond R_H{alpha}_ tend to be lower mass with a few notable exceptions among the
oldest identified clusters.

2. 2004ApJ...608...42S
Re:IC 1613
IC 1613. The first discovery of Cepheids in this galaxy dates back to
the work of Baade and Hubble, later published by Sandage (1971) and
Carlson & Sandage (1990). New BVRI CCD data were published for 11 of the
original 24 Cepheids by Freedman (1988) and were used to derive the
distance modulus listed in column (2) of Table 3. For the purpose of
this paper, we have retained the four Cepheids with a period between 8
and 100 days; periods and VI magnitudes are from Freedman (1988).

3. 2003A&A...401..141L
Re:IC 1613
6.1. 11. IC 1613 Located in the Local Group, IC 1613 is a well-studied
dI whose position is near the celestial equator. The M_HI_/L_B_ value
for IC 1613 is typical for its luminosity compared to other dIs. Its
H II regions have been catalogued by Sandage (1971), Lequeux et
al. (1987), Price et al. (1990), and Hodge et al. (1990). The brightest
HII region was identified by Sandage as #3 (S3), which has been labelled
H II #37 by Hodge et al. (1990). Talent (1980), D'Odorico & Rosa (1982),
and Davidson & Kinman (1982) obtained photoelectric spectrophotometry of
S3, and all three studies showed that the ionization source was a single
Wolf-Rayet (W-R) star. Cole et al. (1999) and Dolphin et al. (2001b)
obtained resolved stellar photometry and derived distances from the tip
of the red giant branch and the red clump, respectively; these distance
measurements are in agreement (730 kpc). Rosado et al. (2001) and
Valdez-Gutierrez et al. (2001) obtained Fabry-Perot interferometry at
H{alpha} and [S 11]{lambda}{lambda}6716,6731 to study the kinematics of
S3 and S8 and found that the nebular emission exhibits two-lobe
structure with superbubbles covering the entire galaxy.
Talent (1980) and Davidson & Kinman (1982) obtained [O III]{lambda}4363
measurements of H II #37, and derived 12+log(O/H) = 7.86 and 7.87,
respectively, and log(N/O) = -1.21 (upper limit) and -0.99, respectively.
Hunter & Gallagher (1985) and Peimbert et al. (1988) measured additional
spectrophotometry for other H II regions, of which one was identified as
a supernova remnant (HII #49, Sandage #8 or S8; D'Odorico et al. 1980;
Rosado et al. 2001). For H II #49, D'Odorico & Dopita (1983) derived
12+log(O/H) = 7.60 and log(N/O) = -0.90, while Peimbert et al. (1988)
derived 12+log(O/H) = 7.83 and log(N/O) = -1.15.
Our spectrum of HII #37 (Fig. 2) also exhibits broad Wolf-Rayet features
near 4471, 4686, and 5800 {lambda}[angstrom}. Due to a strong [O III],
{lambda}4363 detection, an oxygen abundance of 12+log(O/H) = 7.62
+- 0.05 was derived, which is the adopted value here, and 1.6{sigma}
lower than the [O III],{lambda}4363 abundance (7.70) obtained most
recently by Kingsburgh & Barlow (1995). Our log(N/O) = -1.13+-0.18
value is in agreement with the value (-0.96) obtained by Kingsburgh &
Barlow (1995). Our adopted neon-to-oxygen ratio is log(Ne/O) = -0.60 +-
0.05, which is in rough agreement with determinations by Izotov & Thuan
(1999) for other dwarf galaxies at similar oxygen abundance. A new
spectrum for H II #13 did not reveal [O III],{lambda}4363. Oxygen
abundances and N/O values derived using the bright-line method for H II
regions #13 and #37 are in agreement.

4. 2001ApJ...556...24Z
Re:IC 1613
At 2.2' from the central position, an X-ray source is associated with a SNR
(Lozinskaya et al. 1998). The ROSAT HRI image shows extended emission
characteristic of a galaxy cluster about 6.6' below the center of IC 1613.
This confirms the interpretation of Eskridge (1995), who ascribes the X-ray
source observed with the Einstein IPC (IC 1613 X-1) to a cluster of galaxies
he noticed around this position on an optical image.

5. 1997AstL...23..656G
Re:IC 1613
IC 1613. Sandage and Katem (1976) (photographic photometry); Humphreys (1980)
[a survey of the brightest blue stars that is based on the data of Sandage and
Katem (1976)]. The LF (for B magnitudes) that is based on the data of Sandage
and Katem (1976) was constructed by Hoessel (1986). However, since the survey
of Sandage and Katem (1976) covers approximately a third of the galaxy, we
multiplied all values of the LF by three to estimate V(5). The estimate of V(5)
is unreliable.

6. 1997AstL...23..644G
Re:IC 1613
IC 1613. Friedman (1988b) (Cepheids); Humphreys (1980) (V38, V32, V43), (B42,
A22, A42). The studies on this galaxy are based on the photometry of Sandage
and Katem (1976). So far, there is no complete survey ofred and blue stars in
the entire IC 1613 field.

7. 1994AJ....108.2128C
Re:PGC 003844
PGC 003844 = IC 1613. Note improved position (for the center of the
bar) in Table 5 of 1994AJ....108.2128C.

8. 1976RC2...C...0000d
Re:IC 1613
= DDO 008
Dwarf galaxy in the Local Group.
Description and Dimensions:
Ap. J., 166, 13, 1971.
Ap. J., 166, 13, 1971.
Publ. U.S. Naval Obs., XX, Part IV, 1971.
Vistas in Astr., 14, 207, 1972.
Publ. U.S. Naval Obs., XX, Part IV, 1971.
Ann. Rev. Astr. & Ap., 9, 35, 1971.
Vistas in Astr., 14, 231, 1972.
Photometry: (Variable Stars, Cepheids and Distance Modulus)
Ap. J., 166, 13, 1971.
Ap. J., 191, 603, 1974.
P.A.S.P., 85, 119, 1973.
HI 21cm:
IAU Symp., No. 44, 12, 1972.
HII Regions:
Ap. J., 166, 13, 1971.
Ap. J., 190, 525, 1974.
Bull. A.A.S., 5, 349, 1973.

9. 1973UGC...C...0000N
Re:UGC 00668
Im (de Vaucouleurs), Ir I (Holmberg), Ir V (DDO)

10. 1966AJ.....71..922v
Re:DDO 008
= IC 1613.
Member of Local Group.

11. 1964RC1...C...0000d
Re:IC 1613
Asymmetric. Highly resolved. Very low surface brightness. HII rings and
globular clusters.
Note correction to IC coordinates.
In the Local Group.
Hubble, E.P., Realm of the Nebulae., Plate II, 1936.
B.A.N., 15, 308, 1961.
Medd. Lund, II, 128, 1950.
Medd. Lund, I, 175, 1950.
HII Regions:
Zeit. fur Ap., 50, 168, 1960.
Radio Emission:
P.A.S.P., 72, 368, 1960.
M.N.R.A.S., 123, 279, 1961.
HI Emission:
B.A.N., 15, 307, 1961.

12. 1961Hubbl.B...0000S
Re:IC 1613
Irr I
0ct. 18/19, 1952
10 min
Enlarged 6.0X
This is a well known member of the Local Group. Many
Cepheid variables have been discovered by Baade in IC 1613.
The distance modulus is about 24.0. Note the concentration
of the brightest stars into one corner of the galaxy.
This grouping into large associations is a common
feature of Irr galaxies of the Magellanic Cloud type.

13. 1957HPh....53..275d
Re:IC 1613
(Plate 37)
The residula structure includes the well resolved axial bar
and asymmetrical bright patch, rich in supergiants and
emission objects. Note the characteristic asymmetry.
Compare with the SMC (Plate 36), and And DWARF I (Plate 38).

14. 1918PLicO..13....9C
Re:IC 1613
Described as vF, eeL by, Wolf. There are a number of small nebulae in this
region, but no trace of II 1613 in an exposure of 1h 44m. 33 s.n.

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