Distances of Galaxies from the Apparent Size Distribution of Dark Clouds. II NGC 224, NGC 2841 and NGC 7331

Osman, Anas; Ella, M. S.; Issa, Islam

doi:10.1002/asna.2103030604

Cited by 6 publications

(4 citation statements)

References 6 publications

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“…Previously published distance estimates to NGC 7331 are listed in Table 9. Sersic (1960) and Osman (1982) used the size distributions of H II regions and dust clouds, respectively, to estimate distances, and van den Bergh (1960) used a calibration of luminosity classes. Rubin et al (1965) estimated a velocity distance of 14.4 Mpc derived from a recession velocity of +1082 km/s (corrected only for Galactic rotation) and assuming H 0 = 75 km/s/Mpc.…”

Section: Comparison With Previous Distance Estimatesmentioning

confidence: 99%

TheHubble Space TelescopeExtragalactic Distance Scale Key Project. X. The Cepheid Distance to NGC 7331

Hughes

Han

Hoessel

et al. 1998

ApJ

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The distance to NGC 7331 has been derived from Cepheid variables observed with HST/WFPC2, as part of the Extragalactic Distance Scale Key Project. Multi-epoch exposures in F555W (∼ V ) and F814W (∼ I), with photometry derived independently from DoPHOT and DAOPHOT/ALLFRAME programs, were used to detect a total of 13 reliable Cepheids, with periods between 11 and 42 days. The relative distance moduli between NGC 7331 and the LMC, derived from the V and I magnitudes, imply an extinction to NGC 7331 of A V = 0.47 ± 0.15 mag, and an extinction-corrected distance modulus to NGC 7331 of 30.89 ± 0.14(random) mag, equivalent to a distance of 15.1 +1.0 −0.9 Mpc. There are additional systematic uncertainties in the distance modulus of ±0.12 mag due to the calibration of the Cepheid Period-Luminosity relation, and a systematic offset of +0.05 ± 0.04 mag if we applied the metallicity correction inferred from the M101 results of Kennicutt et al 1998.

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Section: Comparison With Previous Distance Estimatesmentioning

confidence: 99%

TheHubble Space TelescopeExtragalactic Distance Scale Key Project. X. The Cepheid Distance to NGC 7331

Hughes

Han

Hoessel

et al. 1998

ApJ

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“…In Table 4, we list the estimated AKARI FIR luminosities as well as the distances. The distances are taken from Tolstoy et al (1995) for Mrk 71 (NGC 2366), Osman, Ella, & Issa (1982) for NGC 2841, Karachentsev et al (2002) for NGC 2976, and Jurcevic & Butcher (2006) for M 101. For more distant galaxies, we estimate the distance from the Galactocentric velocity (taken from NED) 7 by assuming a Hubble constant of 75 km s −1 Mpc −1 .…”

Section: Total Fir Luminositymentioning

confidence: 99%

Far-Infrared Properties of Blue Compact Dwarf Galaxies Observed with AKARI/Far-Infrared Surveyor (FIS)

Hirashita,

Kaneda,

Onaka

et al. 2008

Preprint

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We report basic far-infrared (FIR) properties of eight blue compact dwarf galaxies (BCDs) observed by AKARI. We measure the fluxes at the four FIS bands (wavelengths of 65 µm, 90 µm, 140 µm, and 160 µm). Based on these fluxes, we estimate basic quantities about dust: dust temperature, dust mass, and total FIR luminosity. We find that the typical dust temperature of the BCD sample is systematically higher than that of normal spiral galaxies, although there is a large variety. The interstellar radiation field estimated from the dust temperature ranges up to 100 times of the Galactic value. This confirms the concentrated star-forming activity in BCDs. The star formation rate can be evaluated from the FIR luminosity as 0.01-0.5 M ⊙ yr −1 . Combining this quantity with gas mass taken from the literature, we estimate the gas consumption timescales (gas mass divided by the star formation rate), which prove to span a wide range from 1 Gyr to 100 Gyr. A natural interpretation of this large variety can be provided by intermittent star formation activity. We finally show the relation between dust-to-gas ratio and metallicity (we utilize our estimate of dust mass, and take other necessary quantities from the literature). There is a positive correlation between dust-to-gas ratio and metallicity as expected from chemical evolution models.

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“…Here we present new far-IR images of the nearby Sb galaxy NGC 2841 and Sc galaxy NGC 2976 taken with the Far-Infrared Surveyor (FIS; Kawada et al 2007) onboard AKARI (Murakami et al 2007). The properties of the observed galaxies are summarized in table 1; the distances to NGC 2841 and NGC 2976 are assumed to be 7.6 Mpc (Osman et al 1982) and 3.6 Mpc (Karachentsev et al 2002), respectively. It is confirmed from table 1 that both spiral galaxies are similar in apparent optical sizes, inclination, and position angles, and thus an ideal combination for comparative research between the different Hubble types.…”

Section: Introductionmentioning

confidence: 99%

Far-Infrared Distributions in Nearby Spiral Galaxies NGC 2841 and NGC 2976 Observed with AKARI/Far-Infrared Surveyor (FIS)

Kaneda¹,

Suzuki²,

Onaka³

et al. 2007

Publications of the Astronomical Society of Japan

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Far-infrared (IR) images of the nearby Sb galaxy NGC 2841 and the Sc galaxy NGC 2976 at wavelengths of 65, 90, 140, and 160 µm have been obtained with the Far-Infrared Surveyor (FIS) onboard AKARI. Both galaxies reveal similar morphologies of dust rings. They are, however, significantly different in the dust temperature: a cold (∼ 21 K) ring for NGC 2841 and a warm (∼ 30 K) ring for NGC 2976, which presumably reflects the difference in the origin of the ring structure for the different Hubble type of the galaxy. In addition to the dust ring structure, a warm dust component is detected from the central region of NGC 2841, which may be attributed to the heating by its Low-Ionization Nuclear Emission-line Region nucleus. As for NGC 2976, an extended dust component is observed along the minor axis, which shows a distribution somewhat asymmetrical to the galactic disk; this might be associated with the HI bridge in the M81/M82 group that NGC 2976 belongs to. By taking advantage of a wealth of the far-IR bands of the FIS, it is demonstrated that the spectral energy distribution of NGC 2841 is spatially more variable than that of NGC 2976.

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Distances of Galaxies from the Apparent Size Distribution of Dark Clouds. II NGC 224, NGC 2841 and NGC 7331

Abstract: The distances of three Sb galaxies NGC 224, NGC 2841 and NGC 7331 have been determined using the apparent size distribution of dark interstellar clouds in each of them.

Cited by 6 publications

References 6 publications

TheHubble Space TelescopeExtragalactic Distance Scale Key Project. X. The Cepheid Distance to NGC 7331

TheHubble Space TelescopeExtragalactic Distance Scale Key Project. X. The Cepheid Distance to NGC 7331

Far-Infrared Properties of Blue Compact Dwarf Galaxies Observed with AKARI/Far-Infrared Surveyor (FIS)

Far-Infrared Distributions in Nearby Spiral Galaxies NGC 2841 and NGC 2976 Observed with AKARI/Far-Infrared Surveyor (FIS)

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