Three classical Cepheid variable stars in the nuclear bulge of the Milky Way

Matsunaga, Noriyuki; Kawadu, T.; Nishiyama, Shogo; Nagayama, Takahiro; Kobayashi, Naoto; Tamura, Motohide; Bono, G.; Feast, M. W.; Nagata, T.

doi:10.1038/nature10359

Cited by 93 publications

(136 citation statements)

References 38 publications

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“…The direct measurements discussed in Section 3.1 and the nuclear Cepheid distance of Matsunaga et al (2011) are indeed fully consistent with one another, with the Cepheid distance somewhat on the short side.…”

Section: +042supporting

confidence: 74%

“…Combined with Gillessen et al (2009a) 3.2. Galactic Center Cepheids in context Matsunaga et al (2011) used the near-infrared period-luminosity relation of van Leeuwen et al (2007), adopting solar metallicity, calibrated on the basis of Cepheids with parallax-based distances, to determine the distance modulus to three classical Cepheids in the Galactic nucleus. These three objects were found within 40 pc (projected distance) of the central black hole, leading the authors to conclude that R 0 = 7.9 +0.1 −0.2 kpc (see also Bono et al 2013;Matsunaga 2013).…”

Section: +042mentioning

confidence: 99%

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Clustering of Local Group Distances: Publication Bias or Correlated Measurements? Iv. The Galactic Center

Grijs

Bono

2016

ApJS

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Aiming at deriving a statistically well-justified Galactic Center distance, R 0 , and reducing any occurrence of publication bias, we compiled the most comprehensive and most complete database of Galactic Center distances available to date, containing 273 new or revised R 0 estimates published since records began in October 1918 until June 2016. We separate our R 0 compilation into direct and indirect distance measurements. The latter include a large body of estimates that rely on centroid determinations for a range of tracer populations as well as measurements based on kinematic observations of objects at the solar circle, combined with a mass and/or rotational model of the Milky Way. Careful assessment of the Galactic Center distances resulting from orbital modeling and statistical parallax measurements in the Galactic nucleus yields our final Galactic Center distance recommendation of R 0 = 8.3 ± 0.2 (statistical) ± 0.4 (systematic) kpc. The centroid-based distances are in good agreement with this recommendation. Neither the direct measurements nor the post-1990 centroidbased distance determinations suggest that publication bias may be important. The kinematics-based distance estimates are affected by significantly larger uncertainties, but they can be used to constrain the Galaxy's rotation velocity at the solar Galactocentric distance, Θ 0 . Our results imply that the International Astronomical Union-recommended Galactic Center distance (R IAU 0 = 8.5 kpc) needs a downward adjustment, while its Θ 0 recommendation (Θ 0 = 220 km s −1 ) requires a substantial upward revision.

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Section: +042supporting

confidence: 74%

Section: +042mentioning

confidence: 99%

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? Iv. The Galactic Center

Grijs

Bono

2016

ApJS

Self Cite

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“…Thus, GC South might have been formed by small super-wind activity in our Galaxy. Indeed, Matsunaga et al (2011) andYusef-Zadeh et al (2009) claimed that the star formation rate 10 5−7 yr ago in the GC region was higher than the current rate by one order of magnitude (∼0.1 M ⊙ yr −1 ). Assuming a simple initial mass function (Salpeter 1955), 100 SNe of massive stars (>8 M ⊙ ) are possible within ∼10 5 yr.…”

Section: Origin Of the Gc South Plasmamentioning

confidence: 95%

Discovery of the Recombining Plasma in the South of the Galactic Center: A Relic of the Past Galactic Center Activity?

Nakashima

Nobukawa

Uchida

et al. 2013

ApJ

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We report Suzaku results for soft X-ray emission to the south of the Galactic center (GC). The emission (hereafter "GC South") has an angular size of ∼ 42 ′ × 16 ′ centered at (l, b) ∼ (0.• 0, −1.• 4), and is located in the largely extended Galactic ridge Xray emission (GRXE). The X-ray spectrum of GC South exhibits emission lines from highly ionized atoms. Although the X-ray spectrum of the GRXE can be well fitted with a plasma in collisional ionization equilibrium (CIE), that of GC South cannot be fitted with a plasma in CIE, leaving hump-like residuals at ∼2.5 and 3.5 keV, which are attributable to the radiative recombination continua of the K-shells of Si and S, respectively. In fact, GC South spectrum is well fitted with a recombination-dominant plasma model; the electron temperature is 0.46 keV while atoms are highly ionized (kT = 1.6 keV) in the initial epoch, and the plasma is now in a recombining phase at a relaxation scale (plasma density × elapsed time) of 5.3 × 10 11 s cm −3 . The absorption column density of GC South is consistent with that toward the GC region. Thus GC South is likely to be located in the GC region (∼8 kpc distance). The size of the plasma, the mean density, and the thermal energy are estimated to be ∼ 97 pc×37 pc, 0.16 cm −3 , and 1.6 × 10 51 erg, respectively. We discuss possible origins of the recombinationdominant plasma as a relic of past activity in the GC region.

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“…Groenewegen, Udalski & Bono (2008) used NIR data for 39 population II Cepheids in the bulge from the ogle survey; a related work is by Majaess (2010). Matsunaga et al (2011Matsunaga et al ( , 2013 analysed 3 classical Cepheids and 16 type Recent determinations of the distance to the Galactic Center, R0, used for weighted averages and in Fig. 4.…”

Section: Secondary Estimatesmentioning

confidence: 99%

The Galaxy in Context: Structural, Kinematic, and Integrated Properties

Bland-Hawthorn¹,

Gerhard

2016

Annu. Rev. Astron. Astrophys.

1,382

846

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Our Galaxy, the Milky Way, is a benchmark for understanding disk galaxies. It is the only galaxy whose formation history can be studied using the full distribution of stars from faint dwarfs to supergiants. The oldest components provide us with unique insight into how galaxies form and evolve over billions of years. The Galaxy is a luminous (L ) barred spiral with a central box/peanut bulge, a dominant disk, and a diffuse stellar halo. Based on global properties, it falls in the sparsely populated "green valley" region of the galaxy colour-magnitude diagram. Here we review the key integrated, structural and kinematic parameters of the Galaxy, and point to uncertainties as well as directions for future progress. Galactic studies will continue to play a fundamental role far into the future because there are measurements that can only be made in the near field and much of contemporary astrophysics depends on such observations.

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Three classical Cepheid variable stars in the nuclear bulge of the Milky Way

Cited by 93 publications

References 38 publications

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? Iv. The Galactic Center

Clustering of Local Group Distances: Publication Bias or Correlated Measurements? Iv. The Galactic Center

Discovery of the Recombining Plasma in the South of the Galactic Center: A Relic of the Past Galactic Center Activity?

The Galaxy in Context: Structural, Kinematic, and Integrated Properties

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