PENELLOPE: the ESO data legacy program to complement the Hubble UV Legacy Library of Young Stars (ULLYSES) I. Survey presentation and accretion properties of Orion OB1 and $sigma$-Orionis. (arXiv:2103.12446v2 [astro-ph.SR] UPDATED)

PENELLOPE: the ESO data legacy program to complement the Hubble UV Legacy Library of Young Stars (ULLYSES) I. Survey presentation and accretion properties of Orion OB1 and $sigma$-Orionis. (arXiv:2103.12446v2 [astro-ph.SR] UPDATED)
<a href="http://arxiv.org/find/astro-ph/1/au:+Manara_C/0/1/0/all/0/1">C.F. Manara</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Frasca_A/0/1/0/all/0/1">A. Frasca</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Venuti_L/0/1/0/all/0/1">L. Venuti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Siwak_M/0/1/0/all/0/1">M. Siwak</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Herczeg_G/0/1/0/all/0/1">G.J. Herczeg</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calvet_N/0/1/0/all/0/1">N. Calvet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hernandez_J/0/1/0/all/0/1">J. Hernandez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Tychoniec_L/0/1/0/all/0/1">Ł. Tychoniec</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gangi_M/0/1/0/all/0/1">M. Gangi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alcala_J/0/1/0/all/0/1">J.M. Alcalá</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Boffin_H/0/1/0/all/0/1">H. M. J. Boffin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Nisini_B/0/1/0/all/0/1">B. Nisini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Robberto_M/0/1/0/all/0/1">M. Robberto</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Briceno_C/0/1/0/all/0/1">C. Briceno</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Campbell_White_J/0/1/0/all/0/1">J. Campbell-White</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sicilia_Aguilar_A/0/1/0/all/0/1">A. Sicilia-Aguilar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McGinnis_P/0/1/0/all/0/1">P. McGinnis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fedele_D/0/1/0/all/0/1">D. Fedele</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kospal_A/0/1/0/all/0/1">Á. Kóspál</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Abraham_P/0/1/0/all/0/1">P. Ábrahám</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Alonso_Santiago_J/0/1/0/all/0/1">J. Alonso-Santiago</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Antoniucci_S/0/1/0/all/0/1">S. Antoniucci</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Arulanantham_N/0/1/0/all/0/1">N. Arulanantham</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bacciotti_F/0/1/0/all/0/1">F. Bacciotti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Banzatti_A/0/1/0/all/0/1">A. Banzatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Beccari_G/0/1/0/all/0/1">G. Beccari</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benisty_M/0/1/0/all/0/1">M. Benisty</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biazzo_K/0/1/0/all/0/1">K. Biazzo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bouvier_J/0/1/0/all/0/1">J. Bouvier</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cabrit_S/0/1/0/all/0/1">S. Cabrit</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garatti_A/0/1/0/all/0/1">A. Caratti o Garatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Coffey_D/0/1/0/all/0/1">D. Coffey</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Covino_E/0/1/0/all/0/1">E. Covino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dougados_C/0/1/0/all/0/1">C. Dougados</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Eisloffel_J/0/1/0/all/0/1">J. Eislöffel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ercolano_B/0/1/0/all/0/1">B. Ercolano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Espaillat_C/0/1/0/all/0/1">C. C. Espaillat</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Erkal_J/0/1/0/all/0/1">J. Erkal</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Facchini_S/0/1/0/all/0/1">S. Facchini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fang_M/0/1/0/all/0/1">M. Fang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fiorellino_E/0/1/0/all/0/1">E. Fiorellino</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fischer_W/0/1/0/all/0/1">W.J. Fischer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+France_K/0/1/0/all/0/1">K. France</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gameiro_J/0/1/0/all/0/1">J.F. Gameiro</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lopez_R/0/1/0/all/0/1">R. Garcia Lopez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giannini_T/0/1/0/all/0/1">T. Giannini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ginski_C/0/1/0/all/0/1">C. Ginski</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grankin_K/0/1/0/all/0/1">K. Grankin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gunther_H/0/1/0/all/0/1">H.M. Günther</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hartmann_L/0/1/0/all/0/1">L. Hartmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hillenbrand_L/0/1/0/all/0/1">L.A. Hillenbrand</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hussain_G/0/1/0/all/0/1">G.A.J. Hussain</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+James_M/0/1/0/all/0/1">M.M. James</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koutoulaki_M/0/1/0/all/0/1">M. Koutoulaki</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lodato_G/0/1/0/all/0/1">G. Lodato</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mauco_K/0/1/0/all/0/1">K. Maucó</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mendigutia_I/0/1/0/all/0/1">I. Mendigutía</a>, et al. (15 additional authors not shown)

The evolution of young stars and disks is driven by the interplay of several
processes, notably accretion and ejection of material. Critical to correctly
describe the conditions of planet formation, these processes are best probed
spectroscopically. About five-hundred orbits of the Hubble Space Telescope
(HST) are being devoted in 2020-2022 to the ULLYSES public survey of about 70
low-mass (M<2Msun) young (age<10 Myr) stars at UV wavelengths. Here we present
the PENELLOPE Large Program that is being carried out at the ESO Very Large
Telescope (VLT) to acquire, contemporaneous to HST, optical ESPRESSO/UVES
high-resolution spectra to investigate the kinematics of the emitting gas, and
UV-to-NIR X-Shooter medium-resolution flux-calibrated spectra to provide the
fundamental parameters that HST data alone cannot provide, such as extinction
and stellar properties. The data obtained by PENELLOPE have no proprietary
time, and the fully reduced spectra are made available to the whole community.
Here, we describe the data and the first scientific analysis of the accretion
properties for the sample of thirteen targets located in the Orion OB1
association and in the sigma-Orionis cluster, observed in Nov-Dec 2020. We find
that the accretion rates are in line with those observed previously in
similarly young star-forming regions, with a variability on a timescale of days
of <3. The comparison of the fits to the continuum excess emission obtained
with a slab model on the X-Shooter spectra and the HST/STIS spectra shows a
shortcoming in the X-Shooter estimates of <10%, well within the assumed
uncertainty. Its origin can be either a wrong UV extinction curve or due to the
simplicity of this modelling, and will be investigated in the course of the
PENELLOPE program. The combined ULLYSES and PENELLOPE data will be key for a
better understanding of the accretion/ejection mechanisms in young stars.

http://arxiv.org/icons/sfx.gif