On the ionization conditions in the interarm gas of M 33

Benvenuti, P.; D’Odorico, S.

doi:10.1007/3-540-07409-0_124

Cited by 13 publications

(25 citation statements)

References 1 publication

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“…The original value derived by BCD-75 (see Table 5) needs to be increased by ∼15%, which is however within the errors of the analysis (distance, rotation curve). Benvenuti et al (1975).…”

Section: Mass Model M(r) (R ≤ 6 Kpc)mentioning

confidence: 99%

“…The starburst galaxy NGC 2146 of type Sb II pec (Sandage & Tammann 1987), at a distance of 14.5 Mpc (with 1 ≈ 70 pc), is large and massive and has some outstanding features: a distorted outer shape, although three spiral arms seem to be distinguishable (de Vaucouleurs 1950;Burbidge et al 1959;Benvenuti et al 1975); H i tails, at least at the southern side of an extension up to ∼150 kpc (Caspers & Shane 1986;Taramopoulos et al 2001); a large amount of dust concentrated near the center, with part of it visible as a prominent dust lane and dust "fingers" and polarisation of the visible light (Benvenuti et al 1975;Sandage & Bedke 1994;Draper et al 1995); it has relatively high infrared luminosity L IR = 6 × 10 10 L (Sanders et al 1986); a central condensation, a weak ring, and extended and warped emission of molecular gas (CO) inside which the starburst occurs (Jackson & Ho 1988;Young et al 1988); two H 2 O kilo-masers in the starburst region (Tarchi et al 2002), along with radio supernovae, supernova remnants, and ultra-dense H ii regions (Kronberg & Biermann 1981;Tarchi et al 2000); strong nonthermal continuum radiation produced to a large extent by supernova explosions (Lisenfeld et al 1996); X-ray point sources and diffuse X-ray emission (Armus et al 1995;Della Ceca et al 1999;Inui et al 2005); a cone-like outflow along the minor axis (Armus et al 1995;Greve et al 2000); and maybe a stellar bar (Cabrera-Lavers & Garzon 2004). In short, NGC 2146 is a distorted, dusty, and molecule-rich galaxy with a strong central starburst and a superwind driven out along the minor axis.…”

Section: Introductionmentioning

confidence: 99%

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NGC 2146's starburst region and extended structure

Greve¹,

Neininger

Sievers

et al. 2006

A&A

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We present mm-wavelength and optical observations of the starburst region in NGC 2146. This region of ∼4 kpc diameter contains a well-ordered distribution of stars, gas, and dust, and a well-ordered rotation. The possible anomalies found in our observation are a warped CO distribution and an increase in the CO line width at the NW edge of the starburst region. The investigation of a possible encounter or merger origin of the starburst may therefore have to concentrate on the distorted outer structure of the galaxy. There are three large-scale features of ∼20 kpc extent, two of which give the impression of being stellar sub-systems. The third feature is an incomplete and expanding ring of H ii regions and stars, apparently indicating an event that occurred some 300 Myr ago.

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“…The original value derived by BCD-75 (see Table 5) needs to be increased by ∼15%, which is however within the errors of the analysis (distance, rotation curve). Benvenuti et al (1975).…”

Section: Mass Model M(r) (R ≤ 6 Kpc)mentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

NGC 2146's starburst region and extended structure

Greve¹,

Neininger

Sievers

et al. 2006

A&A

View full text Add to dashboard Cite

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“…Spiral galaxies are the main targets in DIG studies, mainly because the DIG is situated above the plane of the disk (e.g., Otte & Dettmar 1999) or in the interarm region ( Benvenuti et al 1976). In the case of the Milky Way, a low density is the main characteristic used to distinguish the DIG.…”

Section: Diffuse Ionized Gasmentioning

confidence: 99%

Diffuse Ionized Gas in Irregular Galaxies. I. GR 8 and ESO 245-G05

Hidalgo-Gámez¹

2006

Astron J

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We have studied the spectral characteristics of the diffuse ionized gas (DIG) in two irregular galaxies with low metallicities and intermediate star formation rates: ESO 245-G05 and GR 8. The [O iii]/H ratio in these galaxies is higher than in the DIG of spiral galaxies but not as high as in other irregular galaxies previously studied, such as IC 10 and NGC 6822. The [N ii]/H and [S ii]/ H ratios have very small values, indicating the absence of shocks as the ionization source for this gas. This ionization can be explained in both galaxies with photon leakage from the H ii regions as the only source. The percentage of photons that have escaped from the H ii regions is small in ESO 245-G05, only 35%, but varies from 35% up to 60% in GR 8. We also investigated whether the differences found between spiral and irregular galaxies in the [O iii]/H and the [N ii]/H ratios are due to differences in the metal content between these types of galaxies. Although the number of galaxies studied is not very large, it can be concluded that the [O iii]/ H ratio is not related to the oxygen content, while the situation is more ambiguous for the [N ii]/ H ratio.

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“…In order to study the kinematics and density of gas in the central region of NGC 2146 in the light of the proposed merger/encounter hypothesis, we have mapped the H i absorption towards the nuclear radio continuum emission using the VLA (1.8‐arcsec resolution = 130 pc) and the Multi‐Element Radio‐Linked Interferometer Network (MERLIN; 0.2‐arcsec resolution = 15 pc). At the distance of NGC 2146 (14.5 Mpc; Benvenuti, Capaccioli & D'Odorico 1975), 1 arcsec is equivalent to 70 pc.…”

Section: Introductionmentioning

confidence: 99%

Neutral hydrogen absorption at the centre of NGC 2146

Tarchi¹,

Greve²,

Peck³

et al. 2004

Monthly Notices of the Royal Astronomical Society

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We present 1.4-GHz H I absorption line observations towards the starburst in NGC 2146, made with the Very Large Array and the Multi-Element Radio-Linked Interferometer Network. The H I gas has a rotating disc/ring structure with column densities between 6 and 18 × 10 21 atom cm −2 . The H I absorption has a uniform spatial and velocity distribution, and does not reveal any anomalous material concentration or velocity in the central region of the galaxy which might indicate an encounter with another galaxy or a far-evolved merger. We conclude that the signs of an encounter causing the starburst should be searched for in the outer regions of the galaxy.

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On the ionization conditions in the interarm gas of M 33

Cited by 13 publications

References 1 publication

NGC 2146's starburst region and extended structure

NGC 2146's starburst region and extended structure

Diffuse Ionized Gas in Irregular Galaxies. I. GR 8 and ESO 245-G05

Neutral hydrogen absorption at the centre of NGC 2146

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