18-19 Feb 2016

OA Bologna - Angela Bragaglia

STELLAR CLUSTERS & SURVEYS Angela Bragaglia

18-19 Feb 2016

The collaboration : topics

OA Bologna - Angela Bragaglia

18-19 Feb 2016

The collaboration : people

OA Bologna - Angela Bragaglia

18-19 Feb 2016

OA Bologna - Angela Bragaglia

BOCCE : a “mini-survey” Bologna Open Clusters Chemical Evolution project INAF-OABO : Angela Bragaglia, Monica Tosi, Paolo Donati, Eugenio Carretta in collaboration with : Gloria Andreuzzi, Andrea Ahumada, Giacomo Beccari, Michele Cignoni, Gianni Marconi, Raffaele Gratton, et al. Ø  Project started long ago (90s) Ø  Photometry / Synthetic CMDs Ø  HR spectroscopy (SARG, Bragaglia et al. 2001 - 2015) Ø  35+ papers (Gozzoli et al. 1996 – Donati et al. 2015b) see http://davide2.bo.astro.it/scientific-activities/stellar-astrophysics/the-bocce-project/

18-19 Feb 2016

OA Bologna - Angela Bragaglia

BOCCE : a “mini-survey” NGC2355 : P: age=0.9 Gyr, (m-M)0=11 (D¤=1.5 kpc, Z=310 pc, RGC=9.4 kpc), E(B-V)=0.14 4196 P. Donati et al. 4200 P. Donati et al. S: [Fe/H]=-0.06±0.04 rms=0.08 a larger impact on reddening and distance modulus than on age, which is less effected.

5 DISCUSSION

Downloaded from http://mnras.oxfordjournals.org/ at Univers

NGC2335 : Donati, Bragaglia, Carretta, D’Orazi,

With the analysis of NGC 2355, both with photometry, to obtain age, distance, and reddening, and with spectroscopy for detailed chemistry, we add another cluster to the homogenous sample of BOCCE clusters. To put NGC 2355 in the context of other OCs studied, we plot in Fig. 9 our results on a compilation of literature data. We took table 13 of Yong, Carney & Friel (2012) as a starting point, but added other clusters analysed in later papers. Then, to have a more homogenous set, we selected only clusters in the BOCCE sample, either because we derived their distance and age (and often, but not necessarily, the chemical abundances) or their composition (but not age and distance). We ended up with 30 selected clusters, for six of which we adopted literature distance and age while all the others have our BOCCE values; 12 of the 30 clusters have only one spectroscopic analysis, 14 have two, and four have three or more. NGC 2355 falls within the distribution of the other clusters abundances. The information on this sample of OCs (clusters, distance, age, metallicity, and selected elemental ratios, and references for these values) is given in Table 13. No homogenization has been done, we report results from the original papers. Tosi, Cusano, Carini (2015b) Classically, OCs have been used distance. to describe the metallicity Figure 10. Metallicity and α-elements distributions with Galactocentric Our value for disc NGC 2355 is indicated by a red star. Orange filled points are Friel clusters 1995;with Magrini Andreuzzi et al. clusters with BOCCE distribution age and RGC , open(e.g. blue squares literature et ageal. and 2009; RGC . Lines connect different metallicity and [α/Fe] values for the same cluster. References for2011; the spectroscopic and photometric papers are in Table 13. L´epine et al. 2011; Yong et al. 2012; Heiter et al. 2014,

18-19 Feb 2016

OA Bologna - Angela Bragaglia

BOCCE : a “mini-survey” BOCCE photometry : 36 old OCs (+10) (HR spectroscopy for 30+) cfr spectroscopic surveys: APOGEE : 29 OCs (300 stars) Gaia-ESO : 35 Ocs (Dec 2015, 1000x stars)

Trumpler5 (Donati et al. 2105a) NGC2355 (Donati et al. 2015b)

18-19 Feb 2016

OA Bologna - Angela Bragaglia

The next level : large surveys Ø  Gaia - see Altavilla, Carretta, Montegriffo, etc Ø  Gaia-ESO - present Ø  WEAVE - future

18-19 Feb 2016

OA Bologna - Angela Bragaglia

Gaia-ESO Survey in a nutshell •  •  •  •  •  •  •  • 

For information : http://www.gaia-eso.eu

PI Randich/Gilmore 450+ researchers 300 VLT nights/5 years FLAMES 105 MW stars 60+ open clusters STD / GCs distributed analysis

18-19 Feb 2016

OA Bologna - Angela Bragaglia

Gaia-ESO Survey in a Nutshell dataflow Gaia-ESO Survey : data flow

18-19 Feb 2016

OA Bologna - Angela Bragaglia

Gaia-ESO Survey in Bologna Angela Bragaglia (WG4 lead, builder) Paolo Donati (builder) Donatella Romano Giuseppe Altavilla Michele Bellazzini Francesco Calura Gabriele Cocozza Giuliana Fiorentino Silvia Ragaini Monica Tosi Elena Pancino, WG5 lead, now in Arcetri Carmela Lardo, now in Liverpool Silvia Marinoni, now at ASDC Michele Cignoni, now at STScI For information : http://www.gaia-eso.eu

18-19 Feb 2016

OA Bologna - Angela Bragaglia

Gaia-ESO Survey & clusters NGC 1817, NGC 2141, Berkeley 81

1243

the observations. The listed coordinates refer to the telescope pointings.

h m s)

000)

2 41 2 57 1 41

Dec. (◦ ′ ′′ ) (J2000)

Date

16 44 30 10 27 27 −00 27 40

2011 October 24 2011 October 21 2011 October 20

B Exp. time (s)

V Exp. time (s)

I Exp. time (s)

Seeing (arcsec)

1, 3 × 5, 3 × 90 1, 3 × 5, 3 × 90 1, 3 × 5, 3 × 90

1, 3 × 5, 3 × 60 1, 3 × 5, 3 × 60 1, 3 × 5, 3 × 60

1, 3 × 5, 3 × 60 1, 3 × 5, 3 × 60 1, 3 × 5, 3 × 60

1 1 1

from BOCCE to Gaia-ESO : e.g. NGC 2141 (Donati et al. 2014) –2– Downloaded from http://mnras.oxfordjournals.org/ at Università di Bologna - Sistema Bibliotecario d'Ateneo on Ja

age=1.9 Gyr, D¤=4.4 kpc, Z=-440 pc E(B-V)=0.36, z=0.008, RGC=12.2 kpc

clusters, NGC 1817, NGC 2141 and Be 81, from left to right. In the last map on the right we highlight the dimension of the ges were downloaded from the DSS SAO catalogue in the GSSS bandpass 6 (V495). North is up and east is left.

LBC@LBT

rved in service mode at the LBT on he Large Binocular Camera (LBC) in . There are two LBCs, one optimized one for the red-IR ones, mounted at T. Each LBC uses four EEV chips three in a row, and the fourth above Fig. 1). The FoV of LBC is equivalent pixel sampling of 0.23 arcsec. The e central chip (#2) of the LBCs CCD ved in the B filter with the LBC-Blue e LBC-Red one. No dithering pattern e log of the observations. The seeing d the airmass of the exposures was in ds were observed to perform our own ousins system.

rrected for bias and flat-field, and the

energy concentration of the instrumental PSF is very good: 80 per cent of the energy is enclosed in a single CCD pixel in the B band and in 2 × 2 pixels in the V, I bands. The brightest stars, saturated in the deepest images, where efficiently recovered from the short exposure images. The weighted average of the independent measures obtained from the different images was adopted as the final values of the instrumental magnitude (basing the weight on the error). More than 200 stars from the Two Micron All Sky Survey (2MASS) catalogue (Skrutskie et al. 2006) where used as astrometric standards to find an accurate astrometric solution and transform the instrumental positions, in pixels, into J2000 celestial coordinates for each chip. To this aim we adopted the code CATAXCORR, developed by Paolo Montegriffo at the INAF – Osservatorio Astronomico di Bologna. The rms scatter of the solution was about 0.1 arcsec in both RA and Dec. We derived the completeness level of the photometry by means of extensive artificial stars experiments following the recipe described in Bellazzini et al. (2002) and adopted in other papers of this series. About 105 artificial stars were used to derive photometric errors and completeness in B, V and I exposures for the central chip. The results are shown in Table 3.

860 stars with FLAMES (60 with UVES)

Fig. 1.— Left: in gray all the objects in the photometric catalogue of Donati et al. 2014;

18-19 Feb 2016

OA Bologna - Angela Bragaglia

Gaia-ESO Survey & clusters

Radial metallicity gradient – GES OCs

?

?

to be analyzed/observed

iDR4 open clusters (22 age 100Myr-5Gyr)

18-19 Feb 2016

OA Bologna - Angela Bragaglia

Radial Gaia-ESO Survey &metallicity clusters gradient – GES OCs age