On the mass-to-light ratio of the local Galactic disc and the optical luminosity of the Galaxy

Flynn, Chris; Holmberg, Johan; Portinari, L.; Fuchs, B.; Jahreiß, H.

doi:10.1111/j.1365-2966.2006.10911.x

Cited by 333 publications

(458 citation statements)

References 57 publications

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“…We adopt ΣR 0 ,gas = 17.0 M⊙ pc −2 from Read (2014) and Σ R 0 ,thick = 7.0 M⊙ pc −2 from Flynn et al (2006). The local surface density of the thin disc can be derived from the total local stellar surface density Σ R 0 ,stellar = 38.0 M⊙ pc −2 estimated by Bovy et al (2013) by subtracting contributions from the thick disc and the stellar halo (Σ R 0 ,halo = 0.6 M⊙ pc −2 ; Flynn et al 2006). Then, for each sub-discs, the central surface density can be calculated from Σ d,0 = ΣR 0 exp(R0/R d + R hole /R0).…”

Section: Galactic Mass Models and The Fit Resultsmentioning

confidence: 99%

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Huang

Liu

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

159

179

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The rotation curve (RC) of the Milky Way out to ∼ 100 kpc has been constructed using ∼ 16, 000 primary red clump giants (PRCGs) in the outer disk selected from the LSS-GAC and the SDSS-III/APOGEE survey, combined with ∼ 5700 halo K giants (HKGs) selected from the SDSS/SEGUE survey. To derive the RC, the PRCG sample of the warm disc population and the HKG sample of halo stellar population are respectively analyzed using a kinematical model allowing for the asymmetric drift corrections and re-analyzed using the spherical Jeans equation along with measurements of the anisotropic parameter β currently available. The typical uncertainties of RC derived from the PRCG and HKG samples are respectively 5-7 km s −1 and several tens km s −1 . We determine a circular velocity at the solar position, V c (R 0 ) = 240 ± 6 km s −1 and an azimuthal peculiar speed of the Sun, V ⊙ = 12.1 ± 7.6 km s −1 , both in good agreement with the previous determinations. The newly constructed RC has a generally flat value of 240 km s −1 within a Galactocentric distance r of 25 kpc and then decreases steadily to 150 km s −1 at r ∼ 100 kpc. On top of this overall trend, the RC exhibits two prominent localized dips, one at r ∼ 11 kpc and another at r ∼ 19 kpc. From the newly constructed RC, combined with other constraints, we have built a parametrized mass model for the Galaxy, yielding a virial mass of the Milky Way's dark matter halo of 0.90 +0.07 −0.08 × 10 12 M ⊙ and a local dark matter density, ρ ⊙,dm = 0.32 +0.02 −0.02 GeV cm −3 .

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Section: Galactic Mass Models and The Fit Resultsmentioning

confidence: 99%

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Huang

Liu

Yuan

et al. 2016

Mon. Not. R. Astron. Soc.

159

179

View full text Add to dashboard Cite

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“…We use the models of Maraston (1998), which are based on the FRANEC isochrones, for solar metallicity to find the change in turn-off mass per year and relate this to a number of stars by assuming a Salpeter initial mass function starting from 0.25 M . For a total original stellar mass in the bulge of 10 10 M (McGaugh 2008; Flynn et al 2006), the stellar death rate as function of age of the burst is shown in Fig. 10.…”

Section: Birth Rate Of Planetary Nebulae In the Bulgementioning

confidence: 99%

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Gęsicki

Zijlstra

Hajduk

et al. 2014

A&A

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Aims. We study the star-formation history of the Galactic bulge, as derived from the age distribution of the central stars of planetary nebulae that belong to this stellar population. Methods. The high resolution imaging and spectroscopic observations of 31 compact planetary nebulae are used to derive their central star masses. We use the Blöcker post asymptotic giant branch (post-AGB) evolutionary models, which are accelerated by a factor of three in this case to better fit the white dwarf mass distribution and asteroseismological masses. Initial-final mass relations (IFMR) are derived using white dwarfs in clusters. These are applied to determine original stellar masses and ages. The age distribution is corrected for observational bias as a function of stellar mass. We predict that there are about 2000 planetary nebulae in the bulge. Results. The planetary nebula population points at a young bulge population with an extended star-formation history. The Blöcker tracks with the cluster IFMR result in ages, which are unexpectedly young. We find that the Blöcker post-AGB tracks need to be accelerated by a factor of three to fit the local white dwarf masses. This acceleration extends the age distribution. We adjust the IFMR as a free parameter to map the central star ages on the full age range of bulge stellar populations. This fit requires a steeper IFMR than the cluster relation. We find a star-formation rate in the Galactic bulge, which is approximately constant between 3 and 10 Gyr ago. The result indicates that planetary nebulae are mainly associated with the younger and more metal-rich bulge populations. Conclusions. The constant rate of star-formation between 3 and 10 Gyr agrees with suggestions that the metal-rich component of the bulge is formed during an extended process, such as a bar interaction.

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“…Corrections for extinction and redshift (i.e., K-corrections) were accomplished as for the TRGB, but using the Im spectral energy distribution of McCall (2004). In computing luminosities from absolute magnitudes, the absolute magnitude of the Sun was adopted to be 3.315 in K s Flynn et al 2006). Note that no corrections for redshift dimming were applied.…”

Section: Amalgamated Sample and Datamentioning

confidence: 99%

Fundamentals of the dwarf fundamental plane

McCall

Văduvescu

Núñez

et al. 2012

A&A

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Aims. Star-forming dwarfs are studied to elucidate the physical underpinnings of their fundamental plane. Processes controlling dynamics are evaluated, connections between quiescent and bursting dwarfs are examined, and the viability of using structural properties of dwarfs to determine distances is assessed. Methods. Deep surface photometry in K s is presented for 19 star-forming dwarfs. The data are amalgamated with previously published observations to create a sample of 66 galaxies suitable for exploring how global properties and kinematics are connected. Results. It is confirmed that residuals in the Tully-Fisher relation are correlated with surface brightness, but that even after accomodating the surface brightness dependence through the dwarf fundamental plane, residuals in absolute magnitude are far larger than expected from observational errors. Rather, a more fundamental plane is identified which connects the potential to HI line width and surface brightness. Residuals correlate with the axis ratio in a way which can be accommodated by recognizing the galaxies to be oblate spheroids viewed at varying angles. Correction of surface brightnesses to face-on leads to a correlation among the potential, line width, and surface brightness for which residuals are entirely attributable to observational uncertainties. The mean mass-to-light ratio of the diffuse component of the galaxies is constrained to be 0.88±0.20 in K s . Blue compact dwarfs lie in the same plane as dwarf irregulars. The dependence of the potential on line width is less strong than expected for virialized systems, but this may be because surface brightness is acting as a proxy for variations in the mass-to-light ratio from galaxy to galaxy. Altogether, the observations suggest that gas motions are predominantly disordered and isotropic, that they are a consequence of gravity, not turbulence, and that the mass and scale of dark matter haloes scale with the amount and distribution of luminous matter. The tight relationship between the potential and observables offers the promise of determining distances to unresolved star-forming dwarfs to an accuracy comparable to that provided by the Tully-Fisher relation for spirals.

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On the mass-to-light ratio of the local Galactic disc and the optical luminosity of the Galaxy

Cited by 333 publications

References 57 publications

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

The Milky Way's rotation curve out to 100 kpc and its constraint on the Galactic mass distribution

Accelerated post-AGB evolution, initial-final mass relations, and the star-formation history of the Galactic bulge

Fundamentals of the dwarf fundamental plane

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