Substructure, supernovae, and time resolved star formation history for Upper Scorpius

Briceño-Morales, Geovanny; Chanamé, Julio

doi:10.48550/arxiv.2205.01735

Cited by 4 publications

(5 citation statements)

References 49 publications

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“…In Orion, the current stellar population with 6D measurements is estimated to cover about 25% of the total number of young stars in the region (Kounkel & Covey 2019). In the other regions, the coverage of our sample is ∼20%-30% (see Luhman et al 2016;Krolikowski et al 2021;Briceño-Morales & 2022).…”

Section: Uncertainties and Biases In Turbulence Traced By Young Starsmentioning

confidence: 92%

Turbulence in Milky Way Star-forming Regions Traced by Young Stars and Gas

Kounkel

et al. 2022

ApJ

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The interstellar medium (ISM) is turbulent over vast scales and in various phases. In this paper, we study turbulence with different tracers in four nearby star-forming regions: Orion, Ophiuchus, Perseus, and Taurus. We combine the APOGEE-2 and Gaia surveys to obtain the full six-dimensional measurements of positions and velocities of young stars in these regions. The velocity structure functions (VSFs) of the stars show a universal scaling of turbulence. We also obtain Hα gas kinematics in these four regions from the Wisconsin H-Alpha Mapper. The VSFs of the Hα are more diverse compared to those of stars. In regions with recent supernova activities, they show characteristics of local energy injections and higher amplitudes compared to the VSFs of stars and of CO from the literature. Such difference in amplitude of the VSFs can be explained by the different energy and momentum transport from supernovae into different phases of the ISM, thus resulting in higher levels of turbulence in the warm ionized phase traced by Hα. In regions without recent supernova activities, the VSFs of young stars, Hα, and CO are generally consistent, indicating well-coupled turbulence between different phases. Within individual regions, the brighter parts of the Hα gas tend to have a higher level of turbulence than the low-emission parts. Our findings support a complex picture of the Milky Way ISM, where turbulence can be driven at different scales and inject energy unevenly into different phases.

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Section: Uncertainties and Biases In Turbulence Traced By Young Starsmentioning

confidence: 92%

Turbulence in Milky Way Star-forming Regions Traced by Young Stars and Gas

Kounkel

et al. 2022

ApJ

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“…In particular, several studies have recently analysed the region of Upper Scorpius finding different groups in this region (e.g. Damiani et al 2019;Kerr et al 2021;Squicciarini et al 2021;Ratzenbock 2022;Briceño-Morales & Chanamé 2022). The phase space (XYZUVW) is the best space to unravel the spatial and kinematic complexity since it avoids problems like projection effects.…”

Section: Groups In the 6d Phase Spacementioning

confidence: 99%

“…Recently, many authors have studied the substructure of the region using the 5D astrometry of Gaia (see e.g. Damiani et al 2019;Kerr et al 2021;Squicciarini et al 2021;Luhman 2022;Ratzenbock 2022;Briceño-Morales & Chanamé 2022). They all agree that Upper Scorpius is not a single population of stars but there is, instead, a rich substructure of different young populations.…”

Section: Introductionmentioning

confidence: 99%

The star formation history of Upper Scorpius and Ophiuchus

Miret-Roig

Galli

Olivares

et al. 2022

A&A

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Context. Understanding how star formation begins and propagates through molecular clouds is a fundamental but still open question. One major difficulty in addressing this question is the lack of precise 3D kinematics and age information of young stellar populations. Thanks to Gaia's astrometry, large spectroscopic surveys, and improved age-dating methods, this picture is changing. Aims. We aim to study spatial and kinematic substructures of the region encompassed by Upper Scorpius and Ophiuchus star forming regions. We want to determine dynamical traceback ages and study the star formation history of the complex. Methods. We combined our spectroscopic observations with spectra in public archives and large radial velocity surveys to obtain a precise radial velocity sample to complement the Gaia astrometry. We used a Gaussian Mixture Model to identify different kinematic structures in the 6D space of positions and velocities. We applied an orbital traceback analysis to estimate a dynamical traceback age for each group and determine the place where it was born. Results. We identified seven different groups in this region. Four groups (ν Sco, β Sco, σ Sco and δ Sco) are part of Upper Scorpius, two groups (ρ Oph and α Sco) are in Ophiuchus, and another group (π Sco) is a nearby young population. We found an age gradient from the ρ Oph group (the youngest) to the δ Sco group ( 5 Myr), showing that star formation was a sequential process for the past 5 Myr. Our traceback analysis shows that Upper Scorpius and ρ Oph groups share a common origin. The closer group of π Sco is probably older, and the traceback analysis suggests that this group and the α Sco group have a different origin, likely related to other associations in the Sco-Cen complex. Conclusions. Our study shows that this region has a complex star formation history that goes beyond the current formation scenario, likely a result of stellar feedback from massive stars, supernovae explosions, and dynamic interactions between stellar groups and the molecular gas. In particular, we speculate that photo-ionisation from the massive δ Sco star could have triggered star formation first in the β Sco group and then in the ν Sco group. The perturbations of stellar orbits due to stellar feedback and dynamical interactions could also be responsible for the 1-3 Myr difference that we found between dynamical traceback ages and isochronal ages.

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“…The estimated mass of the SN progenitor is 16-18 M . Briceños-Morales and Chanamé [65] studied the SN activity in the OB association Upper Scorpius and attribute this runaway star also to the Lupus I cloud and a SN 1.8 Myr ago.…”

Section: Possible Locations Of the Sn Activitymentioning

confidence: 99%

Recent nucleosynthesis in the solar neighbourhood, detected with live radionuclides

Korschinek

2023

Eur. Phys. J. A

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In this article we try to summarize all information, gathered in the last three decades, on short-lived (order of Myr) radionuclides found in the Solar System with interstellar origin, most probably due to stellar processes like supernovae. The most important isotope is $$^{60}$$ 60 Fe, but we discuss also information on $$^{26}$$ 26 Al, $$^{244}$$ 244 Pu and $$^{53}$$ 53 Mn. We describe the environment of the Solar System during the past $$\approx 10$$ ≈ 10 Myr as well as the likely locations where the supernovae occured. Confirming evidence has been found in the composition and energy distribution of galactic cosmic rays. Finally, we discuss the effects that the recent supernova activity might have had on Earth’s climate and biosphere.

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Substructure, supernovae, and time resolved star formation history for Upper Scorpius

Cited by 4 publications

References 49 publications

Turbulence in Milky Way Star-forming Regions Traced by Young Stars and Gas

Turbulence in Milky Way Star-forming Regions Traced by Young Stars and Gas

The star formation history of Upper Scorpius and Ophiuchus

Recent nucleosynthesis in the solar neighbourhood, detected with live radionuclides

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