Metallicity estimates for H II regions in M81

Stauffer, J. R.; Bothun, G. D.

doi:10.1086/113673

Cited by 20 publications

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“…The results shown in Figs. 3 and 4, and Tables 7, 9, and 10 illustrate the well-known fact that gradient determi- References: (1) Stauffer & Bothun (1984), (2) , (3) nations are very sensitive to the method, to the number of objects used, and to the range of galactocentric distances covered by these objects.…”

Section: Comparison With Other Workmentioning

confidence: 86%

“…This galaxy belongs to an interacting group of galaxies and has well-defined spiral arms that contain a large number of H ii regions. The oxygen abundance gradient of M81 has been calculated in different studies using several methods (Stauffer & Bothun 1984;Pilyugin et al 2004;Stanghellini et al 2010;Patterson et al 2012;Stanghellini et al 2014;Pilyugin, Grebel & Kniazev 2014). These works find slopes that go from −0.093 to −0.011 dex kpc −1 , and some of them include H ii regions where it is possible to measure the electron temperature and calculate the metallicity with the direct method.…”

Section: Introductionmentioning

confidence: 99%

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The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

Arellano-Córdova

Rodríguez

Mayya

et al. 2015

Mon. Not. R. Astron. Soc.

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We study the sensitivity of the methods available for abundance determinations in H ii regions to potential observational problems. We compare the dispersions they introduce around the oxygen and nitrogen abundance gradients when applied to five different sets of spectra of H ii regions in the galaxy M81. Our sample contains 116 H ii regions with galactocentric distances of 3 to 33 kpc, including 48 regions observed by us with the OSIRIS long-slit spectrograph at the 10.4-m Gran Telescopio Canarias telescope. The direct method can be applied to 31 regions, where we can get estimates of the electron temperature. The different methods imply oxygen abundance gradients with slopes of −0.010 to −0.002 dex kpc −1 , and dispersions in the range 0.06-0.25 dex. The direct method produces the shallowest slope and the largest dispersion, illustrating the difficulty of obtaining good estimates of the electron temperature. Three of the strong-line methods, C, ONS, and N2, are remarkably robust, with dispersions of ∼ 0.06 dex, and slopes in the range −0.008 to −0.006 dex kpc −1 . The robustness of each method can be directly related to its sensitivity to the line intensity ratios that are more difficult to measure properly. Since the results of the N2 method depend strongly on the N/O abundance ratio and on the ionization parameter, we recommend the use of the C and ONS methods when no temperature estimates are available or when they have poor quality, although the behaviour of these methods when confronted with regions that have different properties and different values of N/O should be explored.

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Section: Comparison With Other Workmentioning

confidence: 86%

Section: Introductionmentioning

confidence: 99%

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

Arellano-Córdova

Rodríguez

Mayya

et al. 2015

Mon. Not. R. Astron. Soc.

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“…Reference NGC 1090 SDSS NGC 1097 Phillips et al (1984), Storchi-Bergmann et al (1996b) NGC 1232 van , Bresolin et al (2005) NGC 1313 Pagel et al (1980), , Hadfield & Crowther (2007) NGC 1365 Pagel et al (1979), Alloin et al (1981), , Bresolin et al (2005) NGC 1512 Bresolin et al (2012) NGC 1598 NGC 2336 Gusev et al (2012) NGC 2403 Smith (1975), McCall et al (1985), Fierro et al (1986), Garnett et al (1997, Bresolin et al (1999), Garnett et al (1999), Esteban et al (2009) Stauffer & Bothun (1984), Garnett & Shields (1987), Bresolin et al (1999) Smith (1975), Hawley (1978), Sedwick & Aller (1981), Rayo et al (1982), Skillman (1985), McCall et al (1985), Torres-Peimbert et al (1989), Kinkel & Rosa (1994), Garnett & Kennicutt (1994), Kennicutt & Garnett (1996) NGC 7331 Bresolin et al (1999), Gusev et al (2012) NGC 7495 Sánchez et al (2012) NGC 7518 Robertson et al (2012) NGC 7529 Robertson et al (2012) NGC 7570 Sánchez et al (2012) NGC 7591 Robertson et al (2012) NGC 7678 Gusev et al (2012) NGC 7793 , , McCall et al (1985), Bibb...…”

Section: Galaxymentioning

confidence: 99%

The Abundance Properties of Nearby Late-Type Galaxies. I. The Data

2014

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We investigate the oxygen and nitrogen abundance distributions across the optical disks of 130 nearby late-type galaxies using around 3740 published spectra of H ii regions. We use these data in order to provide homogeneous abundance determinations for all objects in the sample, including H ii regions in which not all of the usual diagnostic lines were measured. Examining the relation between N and O abundances in these galaxies we find that the abundances in their centres and at their isophotal R 25 disk radii follow the same relation. The variation in N/H at a given O/H is around 0.3 dex. We suggest that the observed spread in N/H may be partly caused by the time delay between N and O enrichment and the different star formation histories in galaxies of different morphological types and dimensions. We study the correlations between the abundance properties (central O and N abundances, radial O and N gradients) of a galaxy and its morphological type and dimension.

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“…It is useful as the first galaxy to study in our program, since many studies have been made of the structure and star-forming regions of M81, as well as of its nucleus (e.g., Keel 1989;Hill et al 1992;Adler & Westpfahl 1996;Davidge & Courteau 1999;Grossan et al 2001). The H ii regions of M81 have been studied by Hodge & Kennicutt (1983a, 1983b, Stauffer & Bothun (1984), Kaufman, Kennicutt, & Bash (1986), Kaufman et al (1987), Garnett & Shields (1987), Petit, Sivan, & Karachentsev (1988), and Devereux, Jacoby, & Ciardullo (1995). However, the existing optical photometry of the H ii regions is photographic (Kaufman et al 1986;Petit et al 1988, hereafter PSK88), which is not sufficiently accurate for H + [N ii] flux determinations.…”

Section: Introductionmentioning

confidence: 99%

H+[Nii] Observations of the HiiRegions in M81

et al. 2003

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In a first of a series of studies of the H + [N ii] emission from nearby spiral galaxies, we present measurements of H + [N ii] emission from H ii regions in M81. Our method uses large-field CCD images and longslit spectra and is part of the ongoing Beijing-Arizona-Taipei-Connecticut Sky Survey (the BATC survey). The CCD images are taken with the National Astronomical Observatories of China (NAOC) 0.6/0.9 m f/3 Schmidt telescope at the Xinglong Observing Station, using a multicolor filter set. Spectra of 10 of the brightest H ii regions are obtained using the NAOC 2.16 m telescope with a Tek 1024 Â 1024 CCD. The continua of the spectra are calibrated by flux-calibrated images taken from the Schmidt observations. We determine the continuum component of our H + [N ii] image via interpolation from the more accurately measured backgrounds (M81 starlight) obtained from the two neighboring (in wavelength) BATC filter images. We use the calibrated fluxes of H + [N ii] emission from the spectra to normalize this interpolated, continuumsubtracted H + [N ii] image. We estimate the zero-point uncertainty of the measured H + [N ii] emission flux to be $8%. A catalog of H + [N ii] fluxes for 456 H ii regions is provided, with those fluxes being on a more consistent linear scale than previously available. The logarithmically binned H + [N ii] luminosity function of H ii regions is found to have slope = À0.70, consistent with previous results (which allowed = À0.5 to À0.8). From the overall H + [N ii] luminosity of the H ii regions, the star formation rate of M81 is found to be $0.68 M yr À1 , modulo uncertainty with extinction corrections.

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Metallicity estimates for H II regions in M81

Cited by 20 publications

References 0 publications

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

The oxygen abundance gradient in M81 and the robustness of abundance determinations in H ii regions

The Abundance Properties of Nearby Late-Type Galaxies. I. The Data

H+[Nii] Observations of the HiiRegions in M81

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