A5034796189- Stellar, planetary, and galactic studies
- Astrophysics and Star Formation Studies
- Astro and Planetary Science
- Astronomy and Astrophysical Research
- Astronomical Observations and Instrumentation
- Adaptive optics and wavefront sensing
- Spectroscopy and Laser Applications
- Molecular Spectroscopy and Structure
University of Amsterdam
2019-2023
Astronomical Institute of the Slovak Academy of Sciences
2023
Our current understanding is that intermediate- to high-mass stars form in a way similar low-mass stars, through disk accretion. The expected shorter formation timescales, higher accretion rates, and increasingly strong radiation fields compared their lower-mass counterparts may lead significantly different physical conditions play role formation, evolution, the possibility of (sub)stellar companion therein. We searched for mm four ($4-10$ young stellar objects (YSOs) giant H ii region M17...
The majority of massive stars (> 8 M ⊙ ) in OB associations are found close binary systems. Nonetheless, the formation mechanism these binaries is not understood yet. Using literature data, we measured radial-velocity dispersion ( σ 1D as a proxy for fraction ten Galaxy and Large Magellanic Cloud, spanning an age range from 1 to 6 Myr. We find positive trend this with cluster’s age, which consistent hardening. Assuming universal f bin = 0.7, converted behavior evolution minimum orbital...
The young massive-star-forming region M17 contains optically visible massive pre-main-sequence stars that are surrounded by circumstellar disks. Such disks expected to disappear when these reach the main sequence. physical and dynamical structure of remnant poorly constrained, especially inner regions where accretion, photo-evaporation, companion formation migration may be ongoing. We aim constrain properties parts stellar objects B243 (6 Msun) B331 (12 Msun), two systems for which central...
Context. Recently much progress has been made in probing the embedded stages of massive star formation, pointing to formation scenarios that are reminiscent a scaled-up version low-mass formation. However, latest massive-star have rarely observed, as young stars assumed reveal their photospheres only when they fully formed. Aims. Using first and second overtone CO bandhead emission near- mid-infrared photometry, we aim characterize remnant disks around five unique pre-main-sequence (PMS)...
Context . The outcome of the formation massive stars is an important anchor point in and evolution process these stars. It provides insight into physics assembly process, sets conditions for stellar evolution. For stars, rarely observed because processes involved unfold deep down highly extincted molecular clouds. Aims We characterize a population reddened very young star-forming region M17. group 18 O4.5 to B9 constitutes one best samples almost zero-age main-sequence (ZAMS) high-...
Significant progress has been made toward understanding the formation of massive ($M > 8~$M$_{\odot}$) binaries in close orbits. For example, detection a very low velocity dispersion among stars young region M17 and measurement positive trend with age Galactic clusters. The observed could be explained either by lack this or larger binary separations than typically observed, but fraction similar to other latter implies that over time, components migrate each other. We aim determine origin...
Context. The identification and characterisation of populations young massive stars in (giant) H II regions provides important constraints on (i) the formation process their early feedback environment, (ii) initial conditions for population synthesis models predicting evolution ensembles stars. Aims. We identify characterise stellar following giant regions: M 8, G333.6−0.2, NGC 6357. Methods. have acquired - K -band spectra around 200 using Multi Object Spectrograph ESO Very Large Telescope....
Context . It is a challenge to study the formation process of massive stars: their time short, there are only few them, they often deeply embedded, and lie at relatively large distances. Our strategy outcome star search for signatures that remain formation. We have access unique sample (massive) pre-main-sequence (PMS) stars in giant H II region M17. These PMS can be placed on tracks Hertzsprung–Russell diagram (HRD) as we detect photospheric spectrum, exhibit spectral features indicative...
The outcome of the formation massive stars is an important anchor point in their evolution. It provides insight into physics assembly process, and sets conditions for stellar We characterize a population 18 highly reddened O4.5 to B9 very young star-forming region M17. Their properties allow us identify empirical location ZAMS, rotation mass-loss rate there. performed quantitative spectroscopic modeling VLT/X-shooter spectra using NLTE atmosphere code Fastwind fitting approach Kiwi-GA....
Our current understanding is that intermediate- to high-mass stars form in a way similar low-mass stars, is, through disk accretion. However, the physical conditions play role formation, evolution, and possibility of (sub)stellar companion are significantly different. We search for mm counterparts four (4-10 Solar mass) young stellar objects (YSOs) giant Hii region M17 at distance 1.7 kpc. These expose their photospheric spectrum such location on pre-main-sequence (PMS) well established....
Recently much progress has been made in probing the embedded stages of massive star formation, pointing to formation scenarios akin a scaled up version low-mass formation. However, latest have rarely observed. Using 1st and 2nd overtone CO bandhead emission near- mid-infrared photometry we aim characterize remnant disks around 5 unique pre-main-sequence (PMS) stars with masses $6-12~\rm M_{\odot}$, that constrained stellar parameters thanks their detectable photospheres. We seek understand...
It is a challenge to study the formation process of massive stars: their time short, they are few, often deeply embedded, and at relatively large distances. Our strategy outcome star look for signatures remnant formation. We have access unique sample (massive) pre-main-sequence (PMS) stars in giant HII region M17, showing photosphere circumstellar disk. The aim determine variability properties hot gaseous disks understand physical origin emission lines identify dominant processes these...