J. Salinas
A5104728933- Astrophysics and Star Formation Studies
- Stellar, planetary, and galactic studies
- Astro and Planetary Science
- Astronomy and Astrophysical Research
- Molecular Spectroscopy and Structure
- Gamma-ray bursts and supernovae
- Superconducting and THz Device Technology
- Quantum Chromodynamics and Particle Interactions
- Cosmology and Gravitation Theories
- Spacecraft and Cryogenic Technologies
- High-Energy Particle Collisions Research
- Scientific Research and Discoveries
- Atmospheric Ozone and Climate
- Spectroscopy and Laser Applications
- Medical Imaging Techniques and Applications
University of Concepción
2024
Context . A crucial aspect in addressing the challenge of measuring core mass function (CMF), that is pivotal for comprehending origin initial (IMF), lies constraining temperatures cores. Aims We aim to measure luminosity, mass, column density and dust temperature star-forming regions imaged by ALMA-IMF large program. These fields were chosen encompass early evolutionary stages massive protoclusters. High angular resolution mapping required capture properties protostellar pre-stellar cores...
High-mass prestellar cores are extremely rare. The search for such objects has long been hindered by small sample sizes, leading to large uncertainties in their lifetimes and the conditions which high-mass stars ($> 8\,M_{\odot}$) form. We leverage ($\sim 580$ cores) detected ALMA-IMF survey identify both protostellar estimate relative lifetimes. use CO SiO outflows introduce a new automated method based on aperture line emission background subtraction systematically detect associated with...
High-mass prestellar cores are extremely rare. Until recently, the search for such objects has been hampered by small sample sizes, leading to large ambiguities in their lifetimes and hence conditions which high-mass stars (rm ≳ 8 ⊙ ) form. Here we leverage (∼,580 cores) detected ALMA-IMF survey identify both protostellar estimate relative lifetimes. We used CO SiO outflows cores. present a new automated method based on aperture line emission background subtraction systematically detect...
ALMA-IMF observed 15 massive protoclusters capturing multiple spectral lines and the continuum emission. Here, we focus on protocluster G351.77 (∼ 2500 estimated from single-dish observations) located at 2 kpc. We trace dense gas emission kinematics with (1-0) ∼,4 kau resolution. estimate an relative abundance of $∼,(1.66 ± 0.46) $. decompose into up to two velocity components, highlighting kinematic complexity in gas. By examining position-velocity (PV) position-position-velocity (PPV)...
The stellar initial mass function (IMF) is critical to our understanding of star formation and the effects young stars on their environment. On large scales, it enables us use tracers such as UV or Hα emission estimate rate a system interpret unresolved clusters across Universe. So far, there little firm evidence large-scale variations IMF, which thus generally considered “universal”. Stars form from cores, now possible core masses compare (CMF) with presumably produces. goal ALMA-IMF...
The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at a matched sensitivity and spatial resolution. We focus on the dense gas kinematics G353.41 protocluster traced by N 2 H + (1−0), with resolution ~0.02 pc. G353.41, distance ~2kpc, is embedded in larger-scale (~8 pc) filament has mass ~2.5 × 10 3 M ⊙ within 1.3 pc . extracted (1−0) isolated line component decomposed it fitting up to three Gaussian velocity components. This allows us identify...
Abstract We use the H41 α recombination line to create templates of millimeter free–free emission in ALMA-IMF continuum maps, which allows us separate it from dust emission. This method complements spectral-index information and extrapolation centimeter-wavelength maps. derived maps estimate properties up 34 H ii regions across protoclusters. The hydrogen ionizing photon rate Q 0 spectral types follow evolutionary trend proposed by Motte et al. youngest protoclusters lack detectable ionized...
The ALMA-IMF Large Program provides multi-tracer observations of 15 Galactic massive protoclusters at matched sensitivity and spatial resolution. We focus on the dense gas kinematics G353.41 protocluster traced by N$_2$H$^+$ (1$-$0), with an resolution $\sim$0.02 pc. G353.41, a distance $\sim$2 kpc, has mass $\sim$2500 M$_{\odot}$ within $1.3\times1.3$ pc$^2$. extract isolated line component we decompose it fitting up to 3 Gaussian velocity components. This allows us identify structures that...
We use the H$41\alpha$ recombination line to create templates of millimeter free-free emission in ALMA-IMF continuum maps, which allows separate it from dust emission. This method complements spectral-index information and extrapolation centimeter wavelength maps. derived maps estimate properties up 34 HII regions across protoclusters. The hydrogen ionizing-photon rate $Q_0$ spectral types follow evolutionary trend proposed by Motte et al. youngest protoclusters lack detectable ionized gas,...
A crucial aspect in addressing the challenge of measuring core mass function, that is pivotal for comprehending origin initial lies constraining temperatures cores. We aim to measure luminosity, mass, column density and dust temperature star-forming regions imaged by ALMA-IMF large program. High angular resolution mapping required capture properties protostellar pre-stellar cores effectively separate them from larger features, such as dusty filaments. employed point process (PPMAP)...
ALMA-IMF observed 15 massive protoclusters capturing multiple spectral lines and the continuum emission. We focus on G351.77 protocluster ($\sim$ 2500 M$_{\odot}$, estimated from single-dish observations) located at 2 kpc. trace dense gas emission kinematics with N$_2$H$^+$ (1-0) $\sim$ 4 kau resolution. estimate an relative abundance $\sim (1.7 \pm 0.5) \times 10^{-10}$. decompose into up to two velocity components, highlighting kinematic complexity in gas. By examining position-velocity...
The ALMA-IMF Large Program imaged 15 massive protoclusters down to a resolution of sim 2 kau scales, identifying about $10^3$ star-forming cores. mass and luminosity these cores, which are fundamental physical characteristics, difficult determine, problem greatly exacerbated at the distances ge kpc protoclusters. We combined new datasets radiative transfer modeling characterize estimated their mass-averaged temperature masses estimates imply. For one-sixth sample, we measured bolometric...