Clustering of low-mass stars around Herbig Be star IL Cep – evidence of ‘Rocket Effect’ using <i>Gaia</i> EDR3 ?

Mathew, Blesson; Maheswar, G.; Baug, Tapas; Kartha, Sreeja S.; Selvakumar, G.; Manoj, P.; Shridharan, B.; Anusha, R; Narang, Mayank

doi:10.1093/mnras/stab2088

Cited by 5 publications

(5 citation statements)

References 72 publications

Supporting

Mentioning

Contrasting

Order By: Relevance

“…For generating the SED, we used the Johnson U magnitude; B, V, g', r', and i' magnitudes from APASS (Henden et al 2015); G, G RP , and G BP magnitudes from Gaia EDR3; and the infrared J, H, and K s magnitudes from 2MASS. The SED is generated with the python routine used in Arun et al (2021b). From a grid of BT-NextGen (AGSS2009; Hauschildt et al 1999) theoretical stellar atmospheres at solar metallicity and log(g) = 3−4 (since it seems to be evolved from the MS in the CMD), corresponding to various temperatures, we found that the best fit (by means of chi-squared minimization) corresponds to an effective temperature (T eff ) of 20,000 ± 500 K with log(g) of 3.…”

Section: Spectral Energy Distributionmentioning

confidence: 99%

Decoding the X-Ray Flare from MAXI J0709–159 Using Optical Spectroscopy and Multiepoch Photometry

Bhattacharyya¹,

Mathew²,

Ezhikode³

et al. 2022

ApJL

Self Cite

View full text Add to dashboard Cite

We present a follow-up study on the recent detection of two X-ray flaring events by MAXI/Gas Slit Camera observations in soft and hard X-rays from MAXI J0709–159 in the direction of HD 54786 (LY CMa), on 2022 January 25. The X-ray luminosity during the flare was around 1037 erg s−1 (MAXI), which got reduced to 1032 erg s−1 (NuSTAR) after the flare. We took low-resolution spectra of HD 54786 from the 2.01 m Himalayan Chandra Telescope and the 2.34 m Vainu Bappu Telescope (VBT) facilities in India, on 2022 February 1 and 2. In addition to Hα emission, we found emission lines of He i in the optical spectrum of this star. By comparing our spectrum of the object with those from the literature we found that He i lines show variability. Using photometric studies we estimate that the star has an effective temperature of 20,000 K. Although HD 54786 is reported as a supergiant in previous studies, our analysis favors it to be evolving off the main sequence in the color–magnitude diagram. We could not detect any infrared excess, ruling out the possibility of IR emission from a dusty circumstellar disk. Our present study suggests that HD 54786 is a Be/X-ray binary system with a compact object companion, possibly a neutron star.

show abstract

Section: Spectral Energy Distributionmentioning

confidence: 99%

Decoding the X-Ray Flare from MAXI J0709–159 Using Optical Spectroscopy and Multiepoch Photometry

Bhattacharyya¹,

Mathew²,

Ezhikode³

et al. 2022

ApJL

Self Cite

View full text Add to dashboard Cite

show abstract

“…In this work, we report 18 isolated YSOs with M > 10 M e in Gaia astrometric space (four of them from Vioque et al 2022). Regarding the possibility of truly isolated massive star formation (i.e., in the absence of a cluster environment, we note that ∼50%-70% of intermediate-mass YSOs are binaries; Baines et al 2006;Thomas et al 2023), several candidates have been put forward (e.g., Law et al 2022;Fedriani et al 2023), although in-depth analyses have found small clusters around most massive YSOs seemingly isolated (Stephens et al 2017;Arun et al 2021;Yan et al 2023). Similarly, although isolated O stars have been reported (e.g., de Wit et al 2005;Oey et al 2013), this is disputed and it often seems to be a result of observational limitations (Parker & Goodwin 2007;Stephens et al 2017).…”

Section: Comparison With Previous Resultsmentioning

confidence: 90%

“…Previous authors mostly sought clusters in the nearby environments of the intermediate-and high-mass YSOs. This has proven useful in many scientific cases (e.g., Saha et al 2020;Arun et al 2021), but this methodology favors peak-density results in the vicinity of the considered YSOs. In contrast, we have applied a position-independent methodology to the whole Gaia space, without favoring any specific mass range (Section 3).…”

Section: Comparison With Previous Resultsmentioning

confidence: 99%

Clustering Properties of Intermediate and High-mass Young Stellar Objects*

Vioque,

Cavieres,

González

et al. 2023

View full text Add to dashboard Cite

We have selected 337 intermediate- and high-mass young stellar objects (YSOs; 1.5–20 M ⊙) well-characterized with spectroscopy. By means of the clustering algorithm HDBSCAN, we study their clustering and association properties in the Gaia DR3 catalog as a function of stellar mass. We find that the lower-mass YSOs (1.5–4 M ⊙) have clustering rates of 55%–60% in Gaia astrometric space, a percentage similar to that found in the T Tauri regime. However, intermediate-mass YSOs in the range 4–10 M ⊙ show a decreasing clustering rate with stellar mass, down to 27%. We find tentative evidence suggesting that massive YSOs (>10 M ⊙) often (yet not always) appear clustered. We put forward the idea that most massive YSOs form via a mechanism that demands many low-mass stars around them. However, intermediate-mass YSOs form in a classical core-collapse T Tauri way, yet they do not appear often in the clusters around massive YSOs. We also find that intermediate- and high-mass YSOs become less clustered with decreasing disk emission and accretion rate. This points toward an evolution with time. For those sources that appear clustered, no major correlation is found between their stellar properties and the cluster sizes, number of cluster members, cluster densities, or distance to cluster centers. In doing this analysis, we report the identification of 55 new clusters. We tabulated all of the derived cluster parameters for the considered intermediate- and high-mass YSOs.

show abstract

“…This results in the true internal projected motions of these candidate YSOs. A similar approach was followed in other recent studies also, for example, Sicilia-Aguilar et al ( 2019) and Arun et al (2021). Fig.…”

Section: Introductionmentioning

confidence: 78%

Investigation of rocket effect in bright-rimmed clouds using Gaia EDR3

Saha¹,

Maheswar²,

Ojha³

et al. 2022

Monthly Notices of the Royal Astronomical Society: Letters

Self Cite

View full text Add to dashboard Cite

Bright-rimmed clouds (BRCs) are excellent laboratories to explore the radiation-driven implosion mode of star formation because they show evidence of triggered star formation. In our previous study, BRC 18 has been found to accelerate away from the direction of the ionizing H ii region because of the well known ‘Rocket Effect’. Based on the assumption that both BRC 18 and the candidate young stellar objects (YSOs) are kinematically coupled and using the latest Gaia EDR3 measurements, we found that the relative proper motions of the candidate YSOs exhibit a tendency of moving away from the ionizing source. Using BRC 18 as a prototype, we made our further analysis for 21 more BRCs, a majority of which showed a similar trend. For most of the BRCs, the median angle of the relative proper motion of the candidate YSOs is similar to the angle of on-sky direction from the ionizing source to the central IRAS source of the BRC. Based on Pearson’s and Spearman’s correlation coefficients, we found a strong correlation between these two angles, which is further supported by the Kolmogorov-Smirnov (K−S) test on them. The strong correlation between these two angles supports the ‘Rocket Effect’ in the BRCs on the plane-of-sky.

show abstract

Clustering of low-mass stars around Herbig Be star IL Cep – evidence of ‘Rocket Effect’ using Gaia EDR3 ?

Cited by 5 publications

References 72 publications

Decoding the X-Ray Flare from MAXI J0709–159 Using Optical Spectroscopy and Multiepoch Photometry

Decoding the X-Ray Flare from MAXI J0709–159 Using Optical Spectroscopy and Multiepoch Photometry

Clustering Properties of Intermediate and High-mass Young Stellar Objects*

Investigation of rocket effect in bright-rimmed clouds using Gaia EDR3

Contact Info

Product

Resources

About