CEERS: Increasing Scatter along the Star-forming Main Sequence Indicates Early Galaxies Form in Burstsdoi:10.3847/1538-4357/ad9a6aWe present the star formation rate–stellar mass (SFR–M*) relation for galaxies in the Cosmic Evolution Early Release Science survey at 4.5 ≤ z ≤ 12. We model ...
D.R. Gies, in A Massive Star Odyssey: From Main Sequence to Supernova, IAU Symposium, vol. 212, ed. by K. van der Hucht, A. Herrero, & C. Esteban (2003), IAU Symposium, vol. 212, pp. 91–+ Google Scholar R.W. Hilditch, T.J. Harries, S.A. Bell, Astron. Astrophys. 31...
stars: pre-main sequenceX-rays: starsWe present a study of the structure of the high-mass star-forming region RCW 38 and the spatial distribution of its young stellar population. Spitzer Infrared Array Camera (IRAC) photometry (3-8 渭m) is combined with Two Micron All Sky Survey near-IR...
We combine the inferred SFRs and effective radii measurements to derive the star formation surface densities (Σ<sub>SFR</sub>) and present a 'resolved' version of the star formation main sequence (MS) that appears to hold at subgalactic scales, with similar slope and scatter as the one ...
pre-main-sequence starsstar formationstellar evolutionsubmillimetre astronomy/ star-formation theorysubmillimeter telescope observationmillimeter telescope observationstar-forming regionsprestellar evolutionWe consider the current state of star-formation theory and requirements for millimeter and submillimeter ...
A study of the Young star V1331 Cyg in a compact star forming regionExperimental/ astrophysical jetscircumstellar matterpre-main-sequence stars/ compact star forming regionyoung starhigh resolution imagespeculiar T Tau starnebular environmentcomplex nebular fountain-like structure...
We present a quantitative analysis of the star formation history (SFH) of the Local Group dSph galaxy Leo I, from the information in its Hubble Space Telescope [(V-I),I] color-magnitude diagram (CMD). It reaches the level of the oldest main-sequence turnoffs, and this allows us to ...
We examine the connection between the observed star-forming sequence (SFR M α) and the observed evolution of the stellar mass function in the range 0.2 0.9 at all masses and redshifts because this would result in a much higher number density at 10 ☉) ☉) ☉) > 10.5, greatly improves...
{2}\)but also found that embedded young stellar objects have systematically higher mass accretion rates compared to pre-main sequence stars, suggesting a decrease of\({\dot{M}}_{{\rm{acc}}}\)with evolutionary stage. However, this remained inconclusive due to the lack of optically revealed ...
The initial–final mass relation (IFMR) links the birth mass of a star to the mass of the compact remnant left at its death. While the relevance of the IFMR across astrophysics is universally acknowledged, not all of its fine details have yet been resolv