Star formation

About: Star formation is a research topic. Over the lifetime, 37405 publications have been published within this topic receiving 1808161 citations. The topic is also known as: astrogenesis.

The stellar initial mass function in early-type galaxies from absorption line spectroscopy. ii. results

Abstract: The spectral absorption lines in early-type galaxies contain a wealth of information regarding the detailed abundance pattern, star formation history, and stellar initial mass function (IMF) of the underlying stellar population. Using our new population synthesis model that accounts for the effect of variable abundance ratios of 11 elements, we analyze very high quality absorption line spectra of 38 early-type galaxies and the nuclear bulge of M31. These data extend to 1 μm and they therefore include the IMF-sensitive spectral features Na I, Ca II, and FeH at 0.82 μm, 0.86 μm, and 0.99 μm, respectively. The models fit the data well, with typical rms residuals 1%. Strong constraints on the IMF and therefore the stellar mass-to-light ratio, (M/L)stars, are derived for individual galaxies. We find that the IMF becomes increasingly bottom-heavy with increasing velocity dispersion and [Mg/Fe]. At the lowest dispersions and [Mg/Fe] values the derived IMF is consistent with the Milky Way (MW) IMF, while at the highest dispersions and [Mg/Fe] values the derived IMF contains more low-mass stars (is more bottom-heavy) than even a Salpeter IMF. Our best-fit (M/L)stars values do not exceed dynamically based M/L values. We also apply our models to stacked spectra of four metal-rich globular clusters in M31 and find an (M/L)stars that implies fewer low-mass stars than a MW IMF, again agreeing with dynamical constraints. We discuss other possible explanations for the observed trends and conclude that variation in the IMF is the simplest and most plausible.

The Ultraviolet Spectrum of MS 1512–cB58: An Insight into Lyman-Break Galaxies*

Abstract: We present an intermediate-resolution, high signal-to-noise ratio spectrum of the z = 2.7268 galaxy MS 1512-cB58 obtained with the Low Resolution Imaging Spectrograph (LRIS) on the Keck I telescope and covering the rest frame far-UV from 1150 to 1930 A. Gravitational lensing by a foreground cluster boosts the flux from MS 1512-cB58 by a factor of ~30 and provides the opportunity for a first quantitative study of the physical properties of star-forming galaxies at high redshift. The spectrum we have recorded is very rich in stellar and interstellar features; from our analysis of them, we deduce the following main results. The ultraviolet spectral properties of MS 1512-cB58 are remarkably similar to those of nearby star-forming galaxies and spectral synthesis models based on libraries of O and B stars can reproduce accurately the fine detail of the integrated stellar spectrum. The P Cygni profiles of C IV and N V are best matched by continuous star formation with a Salpeter initial mass function (IMF) extending beyond M = 50 M☉—we find no evidence for either a flatter IMF (at the high-mass end) or an IMF deficient in the most massive stars. There are clues in our data that the metallicity of both the stars and the gas is a few times below solar. Our best estimate, ZcB58 ≈ Z☉, is ≈3 times higher than the typical metallicity of damped Lyα systems at the same redshift, which is consistent with the proposal that the galaxies which dominate the H I absorption cross section are generally forming stars at a slower rate than L* Lyman-break galaxies like MS 1512-cB58. The relative velocities of the stellar lines, interstellar absorption, and H II emission indicate the existence of large-scale outflows in the interstellar medium of MS 1512-cB58, with a bulk outward motion of 200 km s-1 and a mass-loss rate of ≈60 M☉ yr-1, which is roughly comparable to the star formation rate. Such galactic winds seem to be a common feature of starburst galaxies at all redshifts and may well be the mechanism that self-regulates star formation, distributes metals over large volumes, and allows the escape of ionizing photons into the intergalactic medium. We suggest further observations of MS 1512-cB58 that would provide more precise measurements of element abundances and of detailed physical parameters and highlight the need to identify other examples of gravitationally lensed galaxies for a comprehensive study of star formation at early times.

Tidal triggering of starbursts and nuclear activity in galaxies

Abstract: Gas distributed throughout a galaxy responds strongly to the tidal field of a companion during a merger. In some cases dynamical instability will drive a large fraction of the gas into the inner regions of the galaxy. A strong burst of star formation will follow and subsequent evolution may lead to the formation of a black hole. Continued accretion of gas by the black hole may provide sufficient power to explain quasars and nuclear activity in otherwise normal galaxies.

Accretion onto Pre-Main-Sequence Stars

Abstract: Accretion through circumstellar disks plays an important role in star formation and in establishing the properties of the regions in which planets form and migrate. The mechanisms by which protostellar and protoplanetary disks accrete onto low-mass stars are not clear; angular momentum transport by magnetic fields is thought to be involved, but the low-ionization conditions in major regions of protoplanetary disks lead to a variety of complex nonideal magnetohydrodynamic effects whose implications are not fully understood. Accretion in pre-main-sequence stars of masses ≲1M⊙ (and in at least some 2–3-M⊙ systems) is generally funneled by the stellar magnetic field, which disrupts the disk at scales typically of order a few stellar radii. Matter moving at near free-fall velocities shocks at the stellar surface; the resulting accretion luminosities from the dissipation of kinetic energy indicate that mass addition during the T Tauri phase over the typical disk lifetime ∼3 Myr is modest in terms of stellar evo...