J/A+A/402/549 UBVRIHalpha photometry of NGC 3293 (Baume+, 2003)
Photometric study of the young open cluster NGC 3293.
Baume G., Vazquez R.A., Carraro G., Feinstein A.
<Astron. Astrophys. 402, 549 (2003)>
=2003A&A...402..549B 2003A&A...402..549B
ADC_Keywords: Clusters, open ; Photometry, UBVRI ; Photometry, H-alpha
Keywords: galaxy: open clusters and associations: individual: NGC 3293 -
stars: imaging - stars: luminosity function, mass function
Description:
Deep and extensive CCD photometric observations at UBV(RI)cHα
were carried out in the area of the open cluster NGC 3293. The new
data set allows to see the entire cluster sequence down to Mv~+4.5,
revealing that stars with Mv←2 are evolving off the main sequence;
stars with -2<Mv<+2 are located on the main sequence and stars with
Mv>+2 are placed above it. According to our analysis, the cluster
distance is d=2750±250pc (V0-Mv=12.2±0.2) and its nuclear age is
8±1Myr. NGC 3293 contains an important fraction of pre-main sequence
(PMS) stars distributed along a parallel band to the ZAMS with masses
from 1 to 2.5M☉ and a mean contraction age of 10Myr. This last
value does not differ too much from the nuclear age estimate. If we
take into account the many factors that may affect the PMS star
positions on the colour-magnitude diagram, both ages can be perfectly
reconciled. The star formation rate, on the other hand, suggests that
NGC 3293 stars formed surely in one single event, therefore favouring
a coeval process of star formation. Using the Halpha data, we detected
nineteen stars with signs of Halpha emission in the region of NGC
3293, another indication that the star formation process is still
active in the region. The computed initial mass function for the
cluster has a slope of x=1.2±0.2, a bit flatter than the typical
slope for field stars and similar to the values found for other young
open clusters.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table1.dat 150 1690 Photometric catalogue of the NGC 3293 region
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Byte-by-byte Description of file: table1.dat
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Bytes Format Units Label Explanations
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2- 5 I4 --- Seq Identification number (this work)
7- 9 I3 --- TGHH80 [3/133]? Identification number from
Turner et al., 1980AJ.....85.1193T 1980AJ.....85.1193T (1)
12- 13 I2 --- FM80 [2/58]? Identification number from
Feinstein & Marraco, 1980PASP...92..266F 1980PASP...92..266F (2)
16- 17 I2 --- FEAS [2/43]? Identification number from
Feast, 1958MNRAS.118..618F 1958MNRAS.118..618F (1)
19- 21 I3 --- HM [9/541]? Identification number from
Herbst & Miller, 1982AJ.....87.1478H 1982AJ.....87.1478H (1)
23- 28 F6.1 pix Xpos X position in pixels (3)
30- 35 F6.1 pix Ypos Y position in pixels (3)
37- 41 F5.2 mag Vmag V magnitude
43- 44 A2 --- n_Vmag Comments for V magnitude (4)
46- 50 F5.2 mag U-B ? U-B colour index
52- 53 A2 --- n_U-B Comments for U-B index (4)
55- 59 F5.2 mag B-V ? B-V colour index
61- 62 A2 --- n_B-V Comments for B-V index (4)
64- 68 F5.2 mag V-Rc ? V-Rc colour index
70- 71 A2 --- n_V-Rc Comments for V-Rc index (4)
73- 77 F5.2 mag V-Ic ? V-Ic colour index
79- 80 A2 --- n_V-Ic Comments for V-Ic index (4)
82- 86 F5.2 mag Halpha ? Halpha index
88- 89 A2 --- n_Halpha Comments for Halpha index (4)
91- 93 A3 --- Memb Membership assignment (5)
95-103 A9 --- HD HD III/135 identification
105-117 A13 --- CPD CPD I/108 identification
120-122 A3 --- --- [TYC]
123-134 A12 --- TYC Tycho I/239 identification
136-150 A15 --- Other Hipparcos or IRAS identification
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Note (1): For numbers lower than 500, identified as
Cl* NGC 3293 FEAS NNN in Simbad.
For numbers upper than 500 (HM numbers only), WEBDA numbers.
Note (2): Indetified as Cl* NGC 3293 FM NN
Note (3): Scale = 0.813 arsecond / pixel
Note (4): Comments on photometry:
(: ) error larger than 0.05
(::) error larger than 0.10
(FM) data from Feinstein & Marraco, 1980PASP...92..266F 1980PASP...92..266F
(HM) data from Herbst & Miller, 1982AJ.....87.1478H 1982AJ.....87.1478H
(TY) data from Tycho catalog, Cat. I/239
Note (5): Membership assignment:
lm1 = likely member from classical photometric method
pm1 = probable member from classical photometric method
lm2 = likely member from subtraction method
pm2 = probable member from subtraction method
nm = non-member
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Acknowledgements: Gustavo Baume
(End) Patricia Bauer [CDS] 23-Sep-2003