A Geometric Determination of the Distance to the Galactic Center

Eisenhauer, F.; Schödel, R.; Genzel, R.; Ott, Thomas; Tecza, Matthias; Abuter, R.; Eckart, A.; Alexander, Tal

doi:10.1086/380188

Cited by 360 publications

(405 citation statements)

References 25 publications

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“…The WF IRAS 18043−2116 was observed with the Very Large Telescope at Paranal Observatory, Chile, using the K-band grating of the SINFONI integral field spectrograph installed at the 8.2-m UT4 (Eisenhauer et al 2003;Bonnet et al 2004). The source was observed on 2015 May 10, covering the wavelength range 1.95 -2.45 µm with spectral resolution ≈ 4000, using the no optics guide star (noAO) mode.…”

Section: Sinfoni (Vlt) Datamentioning

confidence: 99%

Deep into the Water Fountains

Pérez-Sánchez

Tafoya

López

et al. 2017

A&A

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Context. The formation of large-scale (hundreds to few thousands of AU) bipolar structures in the circumstellar envelopes (CSEs) of post-Asymptotic Giant Branch (post-AGB) stars is poorly understood. The shape of these structures, traced by emission from fast molecular outflows, suggests that the dynamics at the innermost regions of these CSEs does not depend only on the energy of the radiation field of the central star. Aims. Multi-frequency observations towards a group of post-AGB sources known as Water Fountain nebulae can help to constrain the nature of the mechanism responsible for the launching and collimation of the fast molecular outlflows traced by high-velocity features of H 2 O maser emission. Methods. Deep into the Water Fountains is an observational project based on the results of programs carried out with three telescope facilities: The Karl G. Jansky Very Large Array (JVLA), The Australia Telescope Compact Array (ATCA), and the Very Large Telescope (SINFONI-VLT). Results. Here we report the results of the observations towards the WF nebula IRAS 18043−2116: Detection of radio continuum emission in the frequency range 1.5 GHz -8.0 GHz; H 2 O maser spectral features and radio continuum emission detected at 22 GHz, and H 2 ro-vibrational emission lines detected at the near infrared. Conclusions. The high-velocity H 2 O maser spectral features, and the shock-excited H 2 emission detected could be produced in molecular layers which are swept up as a consequence of the propagation of a jet-driven wind. Using the derived H 2 column density, we estimated a molecular mass-loss rate of the order of 10 −9 M yr −1 . On the other hand, if the radio continuum flux detected is generated as a consequence of the propagation of a thermal radio jet, the mass-loss rate associated to the outflowing ionized material is of the order of 10 −5 M yr −1 . The presence of a rotating disk could be a plausible explanation for the mass-loss rates estimated.

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Section: Sinfoni (Vlt) Datamentioning

confidence: 99%

Deep into the Water Fountains

Pérez-Sánchez

Tafoya

López

et al. 2017

A&A

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“…Let us assume the distance from the Sun is 5÷6 kpc (Lockman et al 2007). The Galactic latitude and longitude are equal to b = −2 • .3 and l = 39 • .8, correspondingly, and the distance from the Sun towards the Galactic center 7.5 ÷ 8.5 kpc (see for example Eisenhauer et al (2003) and references therein). We come to the conclusion that SS433 and W50 are situated at a Galactocentric distance of about Fig.…”

Section: Abundancesmentioning

confidence: 99%

The Eastern filament of W50

Abolmasov¹,

Maryeva²,

Burenkov³

2010

Astron Nachr

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The dates of receipt and acceptance should be inserted later Key words ISM: individual (W50) -ISM: kinematics and dynamics -stars: individuals (SS433)We present new spectral (FPI and long-slit) data on the Eastern optical filament of the well known radionebula W50 associated with SS433. We find that on sub-parsec scales different emission lines are emitted by different regions with evidently different physical conditions. Kinematical properties of the ionized gas show evidence for moderately high (V ∼ 100 km s −1 ) supersonic motions. [O III]λ5007 emission is found to be multi-component and differs from lowerexcitation [S II]λ6717 line both in spatial and kinematical properties. Indirect evidence for very low characteristic densities of the gas (n ∼ 0.1 cm −3 ) is found. We propose radiative (possibly incomplete) shock waves in low-density, moderately high metallicity gas as the most probable candidate for the power source of the optical filament. Apparent nitrogen overabundance is better understood if the location of W50 in the Galaxy is taken into account.

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“…where r = | r|, r ⊙ = 8 kpc [15] is the distance of the Sun from the galactic center, a is a scale length and ρ l is the total local (solar neighborhood) dark matter density. In particular, the isothermal density profile corresponds to (α, β, γ) = (2,2,0), the Navarro, Frenk and White (NFW) profile [16] corresponds to (α, β, γ) = (1,3,1) and the Moore et al profile [17] to (α, β, γ) = (1.5,3,1.5).…”

Section: Dark Matter In the Galaxymentioning

confidence: 99%

Indirect signals from light neutralinos in supersymmetric models without gaugino mass unification

et al. 2004

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We examine indirect signals produced by neutralino self-annihilations, in the galactic halo or inside celestial bodies, in the frame of an effective MSSM model without gaugino-mass unification at a grand unification scale. We compare our theoretical predictions with current experimental data of gamma-rays and antiprotons in space and of upgoing muons at neutrino telescopes. Results are presented for a wide range of the neutralino mass, though our discussions are focused on light neutralinos. We find that only the antiproton signal is potentially able to set constraints on very low-mass neutralinos, below 20 GeV. The gamma-ray signal, both from the galactic center and from high galactic latitudes, requires significantly steep profiles or substantial clumpiness in order to reach detectable levels. The up-going muon signal is largely below experimental sensitivities for the neutrino flux coming from the Sun; for the flux from the Earth an improvement of about one order of magnitude in experimental sensitivities (with a low energy threshold) can make accessible neutralino masses close to O, Si and M g nuclei masses, for which resonant capture is operative.

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A Geometric Determination of the Distance to the Galactic Center

Cited by 360 publications

References 25 publications

Deep into the Water Fountains

Deep into the Water Fountains

The Eastern filament of W50

Indirect signals from light neutralinos in supersymmetric models without gaugino mass unification

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