The Extragalactic Distance Database: Color-Magnitude Diagrams

Jacobs, B.A. onder red. van E.; Rizzi, L.; Tully, R. Brent; Shaya, E.; Макаров, Д. И.; Макарова, Л. Н.

doi:10.1088/0004-6256/138/2/332

Cited by 254 publications

(229 citation statements)

References 14 publications

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“…We do not include an analogous estimate for the more metal-rich Galactic globular 47 Tuc, because of large error bars and the need to apply theoretical corrections to infer the real TRGB location from the observed one, due to the paucity of bright RGB stars that bias the TRGB detection (see Bellazzini et al 2004, for details). In the same figure we also display the empirical Rizzi et al (2007) relationship, that has been applied by Jacobs et al (2009) to determine distances to a large sample of galaxies in the Local Volume, and the recent Jang & Lee (2017b) empirical calibration. The slope of the Rizzi et al (2007) relationship was estimated by determining the apparent TRGB magnitude vs colour relation in a sample of galaxies, and averaging the slopes.…”

Section: Theoretical Uncertainties On Trgb Distances: Bolometric Corrmentioning

confidence: 99%

“…It was shown repeatedly that the TRGB luminosity can compete in accuracy with other distance indicators such as Cepheids, surface brightness fluctuation, and the Planetary Nebulae Luminosity Function. It has become a standard rung in the extragalactic dis-tance ladder, and has been used to determine distances of up to 10 Mpc in over 40 cases (Jacobs et al 2009). …”

Section: Introductionmentioning

confidence: 99%

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The brightness of the red giant branch tip

Serenelli

Weiß

Cassisi

et al. 2017

A&A

107

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Context. The brightness of the tip of the Red Giant Branch is a useful reference quantity for several fields of astrophysics. An accurate theoretical prediction is needed for such purposes. Aims. We intend to provide a solid theoretical prediction for it, valid for a reference set of standard physical assumptions, and mostly independent of numerical details. Methods. We examine the dependence on physical assumptions and numerical details, for a wide range of metallicities and masses, and based on two different stellar evolution codes. We adjust differences between the codes to treat the physics as identical as possible. After we have succeeded in reproducing the tip brightness between the codes, we present a reference set of models based on the most up to date physical inputs, but neglecting microscopic diffusion, and convert theoretical luminosities to observed infrared colours suitable for observations of resolved populations of stars and include analytic fits to facilitate their use. Results. We find that consistent use of updated nuclear reactions, including an appropriate treatment of the electron screening effects, and careful time-stepping on the upper red giant branch are the most important aspects to bring initially discrepant theoretical values into agreement. Small, but visible differences remain unexplained for very low metallicities and mass values at and above 1.2 M ⊙ , corresponding to ages younger than 4 Gyr. The colour transformations introduce larger uncertainties than the differences between the two stellar evolution codes. Conclusions. We demonstrate that careful stellar modeling allows an accurate prediction for the luminosity of the Red Giant Branch tip. Differences to empirically determined brightnesses may result either from insufficient colour transformations or from deficits in the constitutional physics. We present the best-tested theoretical reference values to date.

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Section: Theoretical Uncertainties On Trgb Distances: Bolometric Corrmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

The brightness of the red giant branch tip

Serenelli

Weiß

Cassisi

et al. 2017

A&A

107

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“…Located at RA 9 h 55 m 52:7 s and Dec 69°40 0 46 00 [116], M82 is an irregular starburst galaxy at a distance ∼3.52 Mpc from Earth [117]. Its CCSN rate is estimated to be ∼ð2.1 − 20Þ × 10 −2 CCSNe yr −1 [118,119].…”

Section: A Location Of Snementioning

confidence: 99%

“…More realistic models for L ν (see, e.g. [130,131]) suggest that over ∼95% of the total energy in neutrinos is emitted [116][117][118][119] within ∼10 s of core bounce. Given the neutrino observation time, t 0 , we consider a 60 s on-source window, aligned ½−10; 50 s about t 0 .…”

Section: B Analysis Timesmentioning

confidence: 99%

Observing gravitational waves from core-collapse supernovae in the advanced detector era

et al. 2016

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The next galactic core-collapse supernova (CCSN) has already exploded, and its electromagnetic (EM) waves, neutrinos, and gravitational waves (GWs) may arrive at any moment. We present an extensive study on the potential sensitivity of prospective detection scenarios for GWs from CCSNe within 5 Mpc, using realistic noise at the predicted sensitivity of the Advanced LIGO and Advanced Virgo detectors for 2015, 2017, and 2019. We quantify the detectability of GWs from CCSNe within the Milky Way and Large Magellanic Cloud, for which there will be an observed neutrino burst. We also consider extreme GW emission scenarios for more distant CCSNe with an associated EM signature. We find that a three-detector network at design sensitivity will be able to detect neutrino-driven CCSN explosions out to ∼5.5 kpc, while rapidly rotating core collapse will be detectable out to the Large Magellanic Cloud at 50 kpc. Of the phenomenological models for extreme GW emission scenarios considered in this study, such as long-lived bar-mode instabilities and disk fragmentation instabilities, all models considered will be detectable out to M31 at 0.77 Mpc, while the most extreme models will be detectable out to M82 at 3.52 Mpc and beyond.

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“…M 82 is a nearby prototypical starburst galaxy with a distance of ∼3.5 Mpc (Jacobs et al 2009) in the M 81 group of galaxies. It hosts a complicated distribution of different gas phases in both its halo and violently starbursting core.…”

Section: Introductionmentioning

confidence: 99%

M 82 – A radio continuum and polarisation study

Adebahr

Krause

Klein

et al. 2013

A&A

104

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Context. The potential role of magnetic fields and cosmic ray propagation for feedback processes in the early Universe can be probed by studies of local starburst counterparts with an equivalent star-formation rate. Aims. In order to study the cosmic ray propagation and determine the magnetic field strength and dominant loss processes in the nearby prototypical starbursting galaxy M 82, a multi-frequency analysis at four radio wavelengths is presented. Methods. Archival data from the Westerbork Synthesis Radio Telescope (WSRT) was reduced and a new calibration technique introduced to reach the high dynamic ranges needed for the complex source morphology. These data were combined with archival Very Large Array (VLA) data, yielding total power maps at λ3 cm, λ6 cm, λ22 cm, and λ92 cm. Results. The data show a confinement of the emission at wavelengths of λ3/λ6 cm to the core region and a largely extended halo reaching up to 4 kpc away from the galaxy midplane at wavelengths of λ22/λ92 cm up to a sensitivity limit of 90 µJy and 1.8 mJy respectively indicating different physical processes in the core and halo regions. The results are used to calculate the magnetic field strength to 98 µG in the core region and to 24 µG in the halo regions. From the observation of ionisation losses, the filling factor of the ionised medium could be estimated to 2%. This leads to a revised view of the magnetic field distribution in the core region and the propagation processes from the core into the halo regions. Conclusions. We find that the radio emission from the core region is dominated by very dense H -regions and supernova remnants, while the surrounding medium is filled with hot X-ray and neutral gas. Cosmic rays radiating at frequencies higher than 1.4 GHz suffer from high synchrotron and inverse Compton losses in the core region and are not able to reach the halo. Even the cosmic rays radiating at longer wavelengths are only able to build up the observed kpc-sized halo, when several starbursting periods are assumed where the far-infrared and radio luminosity vary by an order of magnitude. These findings, together with the strong correlation between Hα, ionised polycyclic aromatic hydrocarbons (PAH + ), and our radio continuum data, suggest a magnetic field which is frozen into the ionised medium and driven out of the galaxy kinematically.

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The Extragalactic Distance Database: Color-Magnitude Diagrams

Cited by 254 publications

References 14 publications

The brightness of the red giant branch tip

The brightness of the red giant branch tip

Observing gravitational waves from core-collapse supernovae in the advanced detector era

M 82 – A radio continuum and polarisation study

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