Galaxies and Cosmology

Combes, F.; Boissé, Patrick; Mazure, A.; Blanchard, Alain

doi:10.1007/978-3-662-04849-8

Cited by 29 publications

(27 citation statements)

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“…And in that context speculating about new-physics phenomena is fully justified by the observed non-Keplerian features of the rotation curves of galaxies or clusters [183]. These non-Keplerian features are usually interpreted as motivation for introducing dark matter (or other non-quantum-gravity new physics, such as MOND [416]), but, in light of the recent awareness of the possibility of UV/IR mixing, it is legitimate to speculate that they may be at least in part due to quantum-spacetime effects.…”

Section: Infrared Quantum-spacetime Phenomenologymentioning

confidence: 99%

Quantum-Spacetime Phenomenology

Amelino‐Camelia

2013

Living Rev. Relativ.

748

874

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Section: Infrared Quantum-spacetime Phenomenologymentioning

confidence: 99%

Quantum-Spacetime Phenomenology

Amelino‐Camelia

2013

Living Rev. Relativ.

748

874

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“…In typical local spiral galaxies, large-scale H i and CO reservoirs have velocity dispersions of 6-10 km s −1 (Combes et al 2002) which, for temperatures of 10 3-4 K, correspond to M ≈ 1 and h ≈ 100 pc. With these values, our model naturally reproduces the break in SF law observed in entire galaxies and smaller regions (but yet h), as illustrated in Figure 2.…”

Section: Local Spirals and The Small Magellanic Cloudmentioning

confidence: 99%

Star Formation Laws and Thresholds From Interstellar Medium Structure and Turbulence

Renaud

Kraljic

Bournaud

2012

ApJ

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We present an analytical model of the relation between the surface density of gas and star formation rate in galaxies and clouds, as a function of the presence of supersonic turbulence and the associated structure of the interstellar medium (ISM). The model predicts a power-law relation of index 3/2, flattened under the effects of stellar feedback at high densities or in very turbulent media, and a break at low surface densities when ISM turbulence becomes too weak to induce strong compression. This model explains the diversity of star formation laws and thresholds observed in nearby spirals and their resolved regions, the Small Magellanic Cloud, high-redshift disks and starbursting mergers, as well as Galactic molecular clouds. While other models have proposed interstellar dust content and molecule formation to be key ingredients to the observed variations of the star formation efficiency, we demonstrate instead that these variations can be explained by ISM turbulence and structure in various types of galaxies.

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“…Although the visible region is always favored, the nearinfrared is equally important because it reveals stars that remain hidden in the visible by interstellar dust (Combes et al 2002). To extend the library into the near-infrared band, we extract the infrared photometric data from 2MASS, which has mapped the full sky at three near-infrared wavelengths with 10 sensitivity limits of J ¼ 15:8, H ¼ 15:1, and K s ¼ 14:3 mag.…”

Section: Derivation Of Stellar Eigenspectramentioning

confidence: 99%

Empirical Modeling of the Stellar Spectrum of Galaxies

Li¹,

Wang²,

Zhou³

et al. 2005

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An empirical method of modeling the stellar spectrum of galaxies is proposed, based on two successive applications of principal component analysis (PCA). PCA is first applied to the newly available stellar library STELIB, supplemented by the J, H, and K s magnitudes taken mainly from the Two Micron All Sky Survey. Next, the resulting eigenspectra are used to fit the observed spectra of a sample of 1016 galaxies selected from the Sloan Digital Sky Survey Data Release 1 (SDSS DR1). PCA is again applied to the fitted spectra to construct the eigenspectra of galaxies with zero velocity dispersion. The first nine galactic eigenspectra so obtained are then used to model the stellar spectrum of the galaxies in SDSS DR1 and synchronously to estimate the stellar velocity dispersion, the spectral type, the near-infrared spectral energy distribution, and the average reddening. Extensive tests show that the spectra of different types of galaxies can be modeled quite accurately using these eigenspectra. The method can yield stellar velocity dispersion with accuracies better than 10% for the spectra of typical signalto-noise ratios in SDSS DR1.

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Galaxies and Cosmology

Cited by 29 publications

References 0 publications

Quantum-Spacetime Phenomenology

Quantum-Spacetime Phenomenology

Star Formation Laws and Thresholds From Interstellar Medium Structure and Turbulence

Empirical Modeling of the Stellar Spectrum of Galaxies

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