J/A+A/633/A38 EW of 10 solar-type stars of Praesepe (D'Orazi+, 2020)
Stellar population astrophysics (SPA) with the TNG.
Revisiting the metallicity of Praesepe (M44).
D'Orazi, V., Oliva, E., Bragaglia, A., Frasca A., Sanna N., Biazzo K.,
Casali G., Desidera S., Lucatello S., Magrini L., Origlia L.
<Astron. Astrophys. 633, A38 (2020)>
=2020A&A...633A..38D 2020A&A...633A..38D (SIMBAD/NED BibCode)
ADC_Keywords: Clusters, open ; Stars, G-type ; Equivalent widths ; Abundances
Keywords: stars: abundances - stars: solar-type -
open clusters and associations: individual: M 44
Abstract:
Open clusters exquisitely track the Galactic disc chemical properties
and its time evolution; a substantial number of studies and large
spectroscopic surveys focus mostly on the chemical content of
relatively old clusters (age>1Gyr). Interestingly, the less studied
young counterpart populating the solar surrounding has been found to
be solar (at most), with a notable surprising lack of young metal-rich
objects. While there is wide consensus about the moderately
above-solar composition of the Hyades cluster, the metallicity of
Praesepe is still controversial. Recent studies suggest that these two
clusters share identical chemical composition and age, but this
conclusion is disputed. With the aim of reassessing the metallicity of
Praesepe, and its difference (if any) with the Hyades cluster, we
present in this paper a spectroscopic investigation of ten solar-type
dwarf members. We exploited GIARPS at the TNG to acquire
high-resolution, high-quality optical and near-IR spectra and derived
stellar parameters, metallicity ([Fe/H]), light elements, alpha- and
iron-peak elements, by using a strictly differential (line-by-line)
approach. We also analysed in the very same way the solar spectrum and
the Hyades solar analogue HD 28099. Our findings suggest that Praesepe
is more metal-rich than the Hyades, at the level of
[Fe/H]=+0.05±0.01dex, with a mean value of [Fe/H]=+0.21±0.01dex.
All the other elements scale with iron, as expected. This result seems
to reject the hypothesis of a common origin for these two open
clusters. Most importantly, Praesepe is currently the most metal-rich,
young open cluster living in the solar neighbourhood
Description:
GIARPS (the simultaneous observing mode of the spectrographers GIANO
and HARPS-N) at the 3.6m telescope TNG was used to target ten
solar-type dwarfs in the Praesepe cluster (Table 1). Observations were
carried out between December 2018 and January 2019.
The instrument configuration allows us to operate with the HARPS-N
spectrograph (R=115000, λλ=3800-6900Å), and the
GIANO-B near-infrared (NIR) spectrograph (R=50000, 0.97-2.5um).
Equivalent width for different species measured in 10 solar-type stars
in Praesepe (table2.dat).
Stellar parameters and abundances is found in the table stars.dat
(table 1 and 5 of the paper).
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
stars.dat 182 10 Basic information, atmospheric parameters and
[Fe/H] abundances for 10 stars (Tables 1+5)
table2.dat 92 227 EW measurements for our sample stars
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See also:
J/A+A/628/A66 : alpha Persei, Pleiades and Praesepe clusters (Lodieu+, 2019)
J/AJ/132/1517 : Spectroscopy of M dwarfs in Praesepe (Kafka+, 2006)
J/ApJ/784/57 : Photometry and proper motions in Praesepe (Wang+, 2014)
Byte-by-byte Description of file: stars.dat
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Bytes Format Units Label Explanations
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1- 8 A8 --- Star Name of the stars (N2632-NN)
14- 34 A21 --- SName Simbad identifier
36- 37 I2 h RAh Right Ascension (J2000)
39- 40 I2 min RAm Right Ascension (J2000)
42- 45 F4.1 s RAs Right Ascension (J2000)
49 A1 --- DE- Declibation sign (J2000)
50- 51 I2 deg DEd Declination (J2000)
53- 54 I2 arcmin DEm Declination (J2000)
56- 59 F4.1 arcsec DEs Declination (J2000)
61- 66 F6.3 mag Gmag Magnitude G from Gaia
70- 75 F6.3 mag Jmag Magnitude J form 2MASS
80- 85 F6.3 mag Hmag Magnitude H form 2MASS
88- 93 F6.3 mag Kmag Magnitude Ks form 2MASS
97-101 F5.2 km/s RV Radial velocity from this study
103-106 F4.2 km/s e_RV Error on the mean radial velocity
111-114 I4 K Teff Effective temperature
116-118 I3 K e_Teff Error on spectroscopic Teff
122-125 F4.2 [cm/s2] logg Surface gravity (logg)
128-131 F4.2 [cm/s2] e_logg Error on spectroscopic logg
135-138 F4.2 km/s Vt Microturbulence velocity
140-143 F4.2 km/s e_Vt Error on Vt
147-150 F4.2 [-] [Fe/H]I Abundance [Fe/H] from Fe I lines
153-156 F4.2 [-] e1_[Fe/H]I Error on [Fe/H]I due to EW
159-162 F4.2 [-] e2_[Fe/H]I Error on [Fe/H]I due to stellar parameters
167-170 F4.2 [-] [Fe/H]II Abundance [Fe/H] from Fe I lines
174-177 F4.2 [-] e1_[Fe/H]II Error on [Fe/H]II due to EW
179-182 F4.2 [-] e2_[Fe/H]II Error on [Fe/H]II due to stellar parameters
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 7 F7.2 0.1nm lambda Wavelength
9- 12 F4.1 --- Species Atomic number (Z)
15- 20 F6.1 0.1pm EW-star6 ?=9999.9 Equivalent width for star 6
23- 28 F6.1 0.1pm EW-star7 ?=9999.9 Equivalent width for star 7
31- 36 F6.1 0.1pm EW-star8 ?=9999.9 Equivalent width for star 8
39- 44 F6.1 0.1pm EW-star9 ?=9999.9 Equivalent width for star 9
47- 52 F6.1 0.1pm EW-star10 ?=9999.9 Equivalent width for star 10
55- 60 F6.1 0.1pm EW-star25 ?=9999.9 Equivalent width for star 25
63- 68 F6.1 0.1pm EW-star26 ?=9999.9 Equivalent width for star 26
71- 76 F6.1 0.1pm EW-star27 ?=9999.9 Equivalent width for star 27
79- 84 F6.1 0.1pm EW-star28 ?=9999.9 Equivalent width for star 28
87- 92 F6.1 0.1pm EW-star32 ?=9999.9 Equivalent width for star 32
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Acknowledgements:
Valentina D'Orazi, valentina.dorazi(at)inaf.it
References:
Origlia et al., Paper I 2019A&A...629A.117O 2019A&A...629A.117O
Ryde et al., Paper II 2019A&A...631L...3R 2019A&A...631L...3R
(End) Valentina D'Orazi [INAF, Padova], Patricia Vannier [CDS] 04-Jan-2020