Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Articles Article Faculty Publications -Articles Dublin Core The Dublin Core metadata element set is common to all Omeka records, including items, files, and collections. For more information see, http://dublincore.org/documents/dces/. Title A name given to the resource Optical spectroscopy of Gaia detected protostars with DOT: Can we probe protostellar photospheres? Subject The topic of the resource orion; Protostars; star formation Description An account of the resource Optical spectroscopy offers the most direct view of the stellar properties and the accretion indicators. Standard accretion tracers, such as H ? , H ? and Ca II triplet lines, and most photospheric features fall in the optical wavelengths. However, these tracers are not readily observable from deeply embedded protostars because of the large line of sight extinction (Av? 50 100 mag) toward them. In some cases, however, it is possible to observe protostars at optical wavelengths if the outflow cavity is aligned along the line-of-sight that allows observations of the photosphere, or the envelope is very tenuous and thin, such that the extinction is low. In such cases, we not only detect these protostars at optical wavelengths, but also follow up spectroscopically. We have used the HOPS catalog (Furlan et al. in 2016) of protostars in Orion to search for optical counterparts for protostars in the Gaia DR3 survey. Out of the 330 protostars in the HOPS sample, an optical counterpart within 2 ? ? is detected for 62 of the protostars. For 17 out of 62 optically detected protostars, we obtained optical spectra (between 5500 and 8900 using nt Object Spectrograph and Camera (ADFOSC) on the 3.6-m Devasthal Optical Telescope (DOT) and Hanle Faint Object Spectrograph Camera (HFOSC) on 2-m Himalayan Chandra Telescope (HCT). We detect strong photospheric features, such as the TiO bands in the spectra (of 4 protostars), hinting that photospheres can form early in the star-formation process. We further determined the spectral types of protostars, which show photospheres similar to a late M-type. Mass accretion rates derived for the protostars are similar to those found for T-Tauri stars, in the range of 10 - 7 10 - 8M? yr - 1 . 2023, Indian Academy of Sciences. Creator An entity primarily responsible for making the resource Narang M.; Manoj P.; Tyagi H.; Nayak P.K.; Sharma S.; Surya A.; Banerjee B.; Mathew B.; Ghosh A.; Verma A. Source A related resource from which the described resource is derived Journal of Astrophysics and Astronomy, Vol-44, No. 2 Publisher An entity responsible for making the resource available Springer Date A point or period of time associated with an event in the lifecycle of the resource 2023-01-01 Identifier An unambiguous reference to the resource within a given context <a href="https://doi.org/10.1007/s12036-023-09982-4" target="_blank" rel="noreferrer noopener">https://doi.org/10.1007/s12036-023-09982-4</a> <br /><br /><a href="https://www.scopus.com/inward/record.uri?eid=2-s2.0-85176725453&amp;doi=10.1007%2Fs12036-023-09982-4&amp;partnerID=40&amp;md5=d5f6fca7a300b75324e2d8d4852d3157" target="_blank" rel="noreferrer noopener">https://www.scopus.com/inward/record.uri?eid=2-s2.0-85176725453&amp;doi=10.1007%2fs12036-023-09982-4&amp;partnerID=40&amp;md5=d5f6fca7a300b75324e2d8d4852d3157</a> Rights Information about rights held in and over the resource Restricted Access Relation A related resource ISSN: 2506335 Format The file format, physical medium, or dimensions of the resource Online Language A language of the resource English Type The nature or genre of the resource Article Coverage The spatial or temporal topic of the resource, the spatial applicability of the resource, or the jurisdiction under which the resource is relevant Narang M., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research (TIFR), Homi Bhabha Road, Colaba, Mumbai, 400005, India, Academia Sinica Institute of Astronomy and Astrophysics, 11F of Astro-Math Bldg., No.1, Sec. 4, Roosevelt Rd., Taipei, 10617, Taiwan; Manoj P., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research (TIFR), Homi Bhabha Road, Colaba, Mumbai, 400005, India; Tyagi H., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research (TIFR), Homi Bhabha Road, Colaba, Mumbai, 400005, India; Nayak P.K., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research (TIFR), Homi Bhabha Road, Colaba, Mumbai, 400005, India, Institute of Astrophysics, Pontificia Universidad Catolica de Chile, Av. Vicu MacKenna 4860, Santiago, 7820436, Chile; Sharma S., Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, 263 001, India; Surya A., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research (TIFR), Homi Bhabha Road, Colaba, Mumbai, 400005, India; Banerjee B., Department of Astronomy and Astrophysics, Tata Institute of Fundamental Research (TIFR), Homi Bhabha Road, Colaba, Mumbai, 400005, India; Mathew B., Department of Physics and Electronics, CHRIST (Deemed to be University), Bangalore, 560029, India; Ghosh A., Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, 263 001, India; Verma A., Aryabhatta Research Institute of Observational Sciences (ARIES), Manora Peak, Nainital, 263 001, India