Calcium and Phosphorus Requirements for Growing Chicks

Tully, W. C.; Hauge, S. M.; Carrick, C. W.; Roberts, Roy E.

doi:10.3382/ps.0100310

Cited by 8 publications

(9 citation statements)

References 4 publications

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“…The 4 r e regions, which include most of stars in individual galaxies, are suitable for Suzaku analysis considering the point spread function. A larger accumulating region may suffer from a larger systematic uncertainties in the background emis- Tully (1988). b Calculated K-band luminosity from the Two Micron All Sky Survey (2MASS).…”

Section: Data Reduction and Construction Of Spectramentioning

confidence: 99%

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ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITHSUZAKU

Konami

Matsushita

Nagino

et al. 2014

ApJ

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We have analyzed 17 early-type galaxies, 13 ellipticals and 4 S0's, observed with Suzaku, and investigated metal abundances (O, Mg, Si, and Fe) and abundance ratios (O/Fe, Mg/Fe, and Si/Fe) in the interstellar medium (ISM). The emission from each on-source region, which is 4 times effective radius, r e , is reproduced with one-or two-temperature thermal plasma models as well as a multi-temperature model, using APEC plasma code v2.0.1. The multi-temperature model gave almost the same abundances and abundance ratios with the 1T or 2T models. The weighted averages of the O, Mg, Si, and Fe abundances of all the sample galaxies derived from the multitemperature model fits are 0.83 ± 0.04, 0.93±0.03, 0.80 ± 0.02, and 0.80±0.02 solar, respectively, in solar units according to the solar abundance table by Lodders (2003). These abundances show no significant dependence on the morphology and environment. The systematic differences in the derived metal abundances between the version 2.0.1 and 1.3.1 of APEC plasma codes were investigated. The derived O and Mg abundances in the ISM agree with the stellar metallicity within a aperture with a radius of one r e derived from optical spectroscopy. From these results, we discuss the past and present SN Ia rates and star formation histories in early-type galaxies.

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Section: Data Reduction and Construction Of Spectramentioning

confidence: 99%

“…f Redshift from Nasa Extragalactic Database. g Distance from Tully (1988). h X-ray luminosity of the thermal emission in the range of 0.3-2.0 keV within 4re from Nagino & .…”

Section: Data Reduction and Construction Of Spectramentioning

confidence: 99%

ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITHSUZAKU

Konami

Matsushita

Nagino

et al. 2014

ApJ

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“…stellar mass loss; Davis et al 2011a) or is left over from the galaxy formation event itself. NGC 4710 is a member the Virgo Cluster (Kraan-Korteweg 1982) at a distance of 16.8 Mpc (Tully 1988), while NGC 5866 is in a small group including two spirals at a distance of 15.3 Mpc (Tully 1988). However, since NGC 4710 is located in the outskirts of the cluster and the distance between NGC 5866 and its nearest companion is rather large, both galaxies are unlikely to have had recent significant interactions with other galaxies or to have been affected by environmental effects.…”

Section: Introductionmentioning

confidence: 99%

Molecular gas kinematics and line diagnostics in early-type galaxies: NGC 4710 and NGC 5866

Topal¹,

Bureau²,

Davis³

et al. 2016

Mon. Not. R. Astron. Soc.

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We present interferometric observations of CO lines ( 12 CO(1-0, 2-1) and 13 CO(1-0, 2-1)) and dense gas tracers (HCN(1-0), HCO + (1-0), HNC(1-0) and HNCO(4-3)) in two nearby edgeon barred lenticular galaxies, NGC 4710 and NGC 5866, with most of the gas concentrated in a nuclear disc and an inner ring in each galaxy. We probe the physical conditions of a two-component molecular interstellar medium in each galaxy and each kinematic component by using molecular line ratio diagnostics in three complementary ways. First, we measure the ratios of the position-velocity diagrams of different lines, second we measure the ratios of each kinematic component's integrated line intensities as a function of projected position, and third we model these line ratios using a non-local thermodynamic equilibrium radiative transfer code. Overall, the nuclear discs appear to have a tenuous molecular gas component that is hotter, optically thinner and with a larger dense gas fraction than that in the inner rings, suggesting more dense clumps immersed in a hotter more diffuse molecular medium. This is consistent with evidence that the physical conditions in the nuclear discs are similar to those in photo-dissociation regions. A similar picture emerges when comparing the observed molecular line ratios with those of other galaxy types. The physical conditions of the molecular gas in the nuclear discs of NGC 4710 and NGC 5866 thus appear intermediate between those of spiral galaxies and starbursts, while the star formation in their inner rings is even milder.

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“…Extensive CO(1-0) (Tacconi & Young 1989;Walsh et al 2002), CO(2-1) (Leroy et al 2009) and CO(3-2) (Walsh et al 2002) observations of NGC 6946 are available in the literature, and we will present here new data comprising one of the most extensive CO(2-1) maps. More limited mapping of the molecules HCN, HCO and CO also exist in the central regions (Ball et al 1985;Weliachew et al 1988;Bonnarel et al 1988;Ishizuki et al 1990; Regan & Vogel 1995;Nieten et al 1999; Levine et al References: (1) NASA/IPAC Extragalactic Database (NED); (2) Skrutskie et al (2006); (3) Tully (1988); (4) de Blok et al (2008); (5) Tacconi & Young (1989); (6) 2008), and the molecular gas physical properties have been studied in the centre (Walsh et al 2002;Bayet et al 2006) and one position in the arms (Walsh et al 2002). Here, we will extend this analysis to all 8 regions defined in Figure 1.…”

Section: Introductionmentioning

confidence: 99%

Molecular gas properties of the giant molecular cloud complexes in the arms and inter-arms of the spiral galaxy NGC 6946

Topal

Bayet

Bureau

et al. 2013

Monthly Notices of the Royal Astronomical Society

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Combining observations of multiple CO lines with radiative transfer modeling is a very powerful tool to investigate the physical properties of the molecular gas in galaxies. Using new observations as well as literature data, we provide the most complete CO ladders ever generated for eight star-forming regions in the spiral arms and inter-arms of the spiral galaxy NGC 6946, with observations of the CO(1-0), CO(2-1), CO(3-2), CO(4-3), CO(6-5), 13 CO(1-0) and 13 CO(2-1) transitions. For each region, we use the large velocity gradient assumption to derive beam-averaged molecular gas physical properties, namely the gas kinetic temperature (T K ), H 2 number volume density (n(H 2 )) and CO number column density (N (CO)). Two complementary approaches are used to compare the observations with the model predictions: χ 2 minimisation and likelihood. The physical conditions derived vary greatly from one region to the next: T K = 10-250 K, n(H 2 )= 10 2.3 -10 7.0 cm −3 and N (CO)= 10 15.0 -10 19.3 cm −2 . The spectral line energy distribution (SLED) of some of these extranuclear regions indicates a star-formation activity that is more intense than that at the centre of our own Milky Way. The molecular gas in regions with a large SLED turnover transition (J max > 4) is hot but tenuous with a high CO column density, while that in regions with a low SLED turnover transition (J max 4) is cold but dense with a low CO column density. We finally discuss and find some correlations between the physical properties of the molecular gas in each region and the presence of young stellar population indicators (supernova remnants, H II regions, H I holes, etc).

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Calcium and Phosphorus Requirements for Growing Chicks

Cited by 8 publications

References 4 publications

ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITHSUZAKU

ABUNDANCE PATTERNS IN THE INTERSTELLAR MEDIUM OF EARLY-TYPE GALAXIES OBSERVED WITHSUZAKU

Molecular gas kinematics and line diagnostics in early-type galaxies: NGC 4710 and NGC 5866

Molecular gas properties of the giant molecular cloud complexes in the arms and inter-arms of the spiral galaxy NGC 6946

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