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Articles de revues sur le sujet « NGC 6810 »

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Auteur : Grafiati
Publié le 10 mars 2023

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1

Strickland, David K. « A new superwind galaxy : XMM–Newton observations of NGC 6810 ». Monthly Notices of the Royal Astronomical Society 376, no 2 (avril 2007) : 523–33. http://dx.doi.org/10.1111/j.1365-2966.2007.11478.x.

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2

Hekker, S., S. Basu, D. Stello, T. Kallinger, F. Grundahl, S. Mathur, R. A. García et al. « Asteroseismic inferences on red giants in open clusters NGC 6791, NGC 6819, and NGC 6811 usingKepler ». Astronomy & ; Astrophysics 530 (18 mai 2011) : A100. http://dx.doi.org/10.1051/0004-6361/201016303.

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3

Corsaro, Enrico, Dennis Stello, Daniel Huber, Timothy R. Bedding, Alfio Bonanno, Karsten Brogaard, Thomas Kallinger et al. « ASTEROSEISMOLOGY OF THE OPEN CLUSTERS NGC 6791, NGC 6811, AND NGC 6819 FROM 19 MONTHS OFKEPLERPHOTOMETRY ». Astrophysical Journal 757, no 2 (17 septembre 2012) : 190. http://dx.doi.org/10.1088/0004-637x/757/2/190.

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4

Stello, Dennis, Søren Meibom, Ronald L. Gilliland, Frank Grundahl, Saskia Hekker, Benoît Mosser, Thomas Kallinger et al. « AN ASTEROSEISMIC MEMBERSHIP STUDY OF THE RED GIANTS IN THREE OPEN CLUSTERS OBSERVED BYKEPLER : NGC 6791, NGC 6819, AND NGC 6811 ». Astrophysical Journal 739, no 1 (30 août 2011) : 13. http://dx.doi.org/10.1088/0004-637x/739/1/13.

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5

Bellamy, B., et D. Stello. « New Seismic Members in NGC 6791 and NGC 6819 ». EPJ Web of Conferences 101 (2015) : 06007. http://dx.doi.org/10.1051/epjconf/201510106007.

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6

Madejski, Greg M., Chris Done, T. Jane Turner, Richard F. Mushotzky, Peter Serlemitsos, Fabrizio Fiore, Marek Sikora et Mitchell C. Begelman. « Solving the Mystery of the Periodicity in the Seyfert Galaxy NGC 6814 ». Symposium - International Astronomical Union 159 (1994) : 127–30. http://dx.doi.org/10.1017/s0074180900174911.

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The reports of periodic X–ray emission from the Seyfert galaxy NGC 6814 have motivated a number of exotic models for the active nucleus. Our ROSAT observation shows that while the nucleus of NGC 6814 is indeed an X–ray emitter, the periodicity is due to another source, most likely a Galactic accreting binary system, ∼ 37 arc min away.
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7

Ананьевская, Ю. К., В. Н. Фролов et Е. В. Поляков. « Исследование рассеянного звездного скопления NGC 6800 ». Письма в астрономический журнал : Астрономия и космическая астрофизика 41, no 07 (2015) : 367–76. http://dx.doi.org/10.7868/s0320010815060017.

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8

Yontan, T., S. Bilir, Z. F. Bostancı, T. Ak, S. Karaali, T. Güver, S. Ak, Ş. Duran et E. Paunzen. « CCD UBVRI photometry of NGC 6811 ». Astrophysics and Space Science 355, no 2 (29 janvier 2015) : 267–81. http://dx.doi.org/10.1007/s10509-014-2175-5.

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9

Kuehn, Charles A., Jason A. Drury, Beau R. Bellamy, Dennis Stello, Timothy R. Bedding, Mike Reed et Breanna Quick. « Photometry UsingKepler“Superstamps” of Open Clusters NGC 6791 & ; NGC 6819 ». EPJ Web of Conferences 101 (2015) : 06040. http://dx.doi.org/10.1051/epjconf/201510106040.

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10

Pottasch, S. R., D. A. Beintema et W. A. Feibelman. « Abundances of planetary nebulae NGC 2022, NGC 6818 and IC 4191 ». Astronomy & ; Astrophysics 436, no 3 (juin 2005) : 953–65. http://dx.doi.org/10.1051/0004-6361:20042627.

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11

Liszt, Harvey S., et John M. Dickey. « HI Emission From the Seyfert Galaxies NGC 4051 and NGC 6814 ». Astronomical Journal 110 (septembre 1995) : 998. http://dx.doi.org/10.1086/117579.

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12

Abedigamba, O. P., L. A. Balona et T. R. Medupe. « Red Clump stars inKepleropen cluster NGC 6819 ». EPJ Web of Conferences 101 (2015) : 06001. http://dx.doi.org/10.1051/epjconf/201510106001.

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13

Vaidya, Kaushar, Khushboo K. Rao, Manan Agarwal et Souradeep Bhattacharya. « Blue straggler populations of seven open clusters with Gaia DR2 ». Monthly Notices of the Royal Astronomical Society 496, no 2 (12 juin 2020) : 2402–21. http://dx.doi.org/10.1093/mnras/staa1667.

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ABSTRACT Blue straggler stars (BSS) are well studied in globular clusters but their systematic study with secure membership determination is lacking in open clusters. We use Gaia DR2 data to determine accurate stellar membership for four intermediate-age open clusters, namely Melotte 66, NGC 2158, NGC 2506, and NGC 6819, and three old open clusters, namely, Berkeley 39, NGC 188, and NGC 6791, to subsequently study their BSS populations. The BSS radial distributions of five clusters, namely Melotte 66, NGC 188, NGC 2158, NGC 2506, and NGC 6791, show bimodal distributions, placing them with Family II globular clusters that are of intermediate dynamical ages. The location of minima, rmin, in the bimodal BSS radial distributions, varies from 1.5rc to 4.0rc, where rc is the core radius of the clusters. We find a positive correlation between rmin and Nrelax, the ratio of cluster age to the current central relaxation time of the cluster. We further report that this correlation is consistent in its slope, within the errors, with the slope of the globular cluster correlation between the same quantities, but with a slightly higher intercept. This is the first example in open clusters that shows BSS radial distributions as efficient probes of dynamical age. The BSS radial distributions of the remaining two clusters, Berkeley 39 and NGC 6819, are flat. The estimated Nrelax values of these two clusters, however, indicate that they are dynamically evolved. Berkeley 39 especially has its entire BSS population completely segregated to the inner regions of the cluster.
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14

Kuehn, Charles A., Jason Drury, Dennis Stello et Timothy R. Bedding. « Photometry using Kepler “superstamps” of open clusters NGC 6791 & ; NGC 6819 ». Proceedings of the International Astronomical Union 9, S301 (août 2013) : 445–46. http://dx.doi.org/10.1017/s174392131301497x.

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AbstractThe Kepler space telescope has proven to be a gold mine for the study of variable stars. Unfortunately, Kepler only returns a handful of pixels surrounding each star on the target list, which omits a large number of stars in the Kepler field. For the open clusters NGC 6791 and NGC 6819, Kepler also reads out larger superstamps which contain complete images of the central region of each cluster. These cluster images can potentially be used to study additional stars in the open clusters. We present preliminary results from using traditional photometric techniques to identify and analyze additional variable stars from these images.
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15

Bisch, S. M., M. G. Pastoriza, H. Dottori et I. Busko. « A Search for Periodicities in the Light Variation of Some Seyfert Galaxies ». Symposium - International Astronomical Union 121 (1987) : 185–90. http://dx.doi.org/10.1017/s0074180900155093.

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Penfold's UBV observations of the Nuclei of the Seyfert galaxies NGC 1566, NGC 3227, NGC 3783, NGC 6814, NGC 7469, Mk 50 and IC 4329A are examined to look for a possible periodicity in the variation of the magnitudes and colors. A method based on the fitting of sinusoidals and the calculation of the multiple correlation coefficient adequated to the analysis of observations unequally spaced in time is used to analyse the data. Four of the seven galaxies studied show a high probability of having periodic component in the variation. Recent UBV observations were used to test the components in two of them.
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16

Van Cauteren, P. « Search for intrinsic variable stars in three open clusters : NGC 1664, NGC 6811 and NGC 7209 ». Communications in Asteroseismology 146 (2007) : 21–32. http://dx.doi.org/10.1553/cia146s21.

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17

Vennik, Jaan. « Interacting galaxies in the NGC 697 group of galaxies ». Proceedings of the International Astronomical Union 11, S321 (mars 2016) : 300. http://dx.doi.org/10.1017/s1743921316008838.

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AbstractWe studied the morphology of two brightest members of the nearby NGC 697 group of galaxies, and found evidence of satellite accretion onto the primary galaxy NGC 697 of the group as well as outer and inner irregularities of the only early-type galaxy NGC 680 of the group, which are probably shaped by recent dry merging event(s).
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18

Yang, Yong, Chengyuan Li, Yang Huang et Xiaowei Liu. « At What Mass Are Stars Braked ? The Implication from the Turnoff Morphology of NGC 6819 ». Astrophysical Journal 925, no 2 (1 février 2022) : 159. http://dx.doi.org/10.3847/1538-4357/ac3ee2.

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Abstract Extended main-sequence turnoffs (eMSTOs) apparent in most young and intermediate-age clusters (younger than ∼2 Gyr) are known features caused by fast rotating early-type (earlier than F-type) stars. Late-type stars are not fast rotators because their initial angular momenta have been quickly dispersed due to magnetic braking. However, the mass limit below which stars have been magnetically braked has not been well constrained by observation. In this paper, we present an analysis of the eMSTO of NGC 6819, an open cluster of an intermediate-age (∼2.5 Gyr), believed to be comparable to the lifetime of stars near the mass limit for magnetic braking. By comparing the observation with synthetic color–magnitude diagrams, we find that NGC 6819 does not harbor an obvious eMSTO. The morphology of its turnoff region can be readily explained by a simple stellar population considering the observational uncertainties as well as the differential reddening. In addition, the MSTO stars in NGC 6819 have very small values of average rotational velocity and dispersion, indicating that they have undergone significant magnetic braking. Combining with results in the literature for clusters of younger ages, our current work suggests that the critical age for the disappearance of eMSTO in star clusters must be shorter but very close to the age of NGC 6819, and this in turn implies a critical stellar mass for magnetic braking at solar metallicity above but close to 1.54 M ⊙ based on the PARSEC model. We emphasize that the phenomenon of eMSTO could provide an unique way to constrain the onset mass of magnetic braking.
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19

KANG, YaNG-WOO, et HONG BAE ANN. « DYNAMICAL EVOLUTION IN THE OPEN CLUSTER NGC 6819 ». Journal of The Korean Astronomical Society 35, no 2 (1 juin 2002) : 87–95. http://dx.doi.org/10.5303/jkas.2002.35.2.087.

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20

Ananjevskaja, Yu K., V. N. Frolov et E. V. Polyakov. « Investigation of the open star cluster NGC 6800 ». Astronomy Letters 41, no 7 (juillet 2015) : 334–42. http://dx.doi.org/10.1134/s1063773715060018.

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21

Janes, Kenneth, Sydney A. Barnes, Søren Meibom et Sadia Hoq. « NGC 6811 : AN INTERMEDIATE-AGE CLUSTER IN THEKEPLERFIELD ». Astronomical Journal 145, no 1 (6 décembre 2012) : 7. http://dx.doi.org/10.1088/0004-6256/145/1/7.

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22

Lee-Brown, Donald B., Barbara J. Anthony-Twarog, Constantine P. Deliyannis, Evan Rich et Bruce A. Twarog. « SPECTROSCOPIC ABUNDANCES IN THE OPEN CLUSTER NGC 6819 ». Astronomical Journal 149, no 4 (9 mars 2015) : 121. http://dx.doi.org/10.1088/0004-6256/149/4/121.

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23

Balona, L. A., T. Medupe, O. P. Abedigamba, G. Ayane, L. Keeley, M. Matsididi, G. Mekonnen, M. D. Nhlapo et N. Sithole. « Kepler observations of the open cluster NGC 6819 ». Monthly Notices of the Royal Astronomical Society 430, no 4 (20 février 2013) : 3472–82. http://dx.doi.org/10.1093/mnras/stt148.

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24

Yu(俞伯傑), Po-Chieh, Chien-Cheng Lin(林建爭), Hsing-Wen Lin(林省文), Chien-De Lee(李建德), Nick Konidaris, Chow-Choong Ngeow(饒兆聰), Wing-Huen Ip(葉永烜) et al. « Be STARS IN THE OPEN CLUSTER NGC 6830 ». Astronomical Journal 151, no 5 (21 avril 2016) : 121. http://dx.doi.org/10.3847/0004-6256/151/5/121.

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25

Turner, T. J., Christine Done, Richard Mushotzky, Greg Madejski et Hideyo Kunieda. « Evidence for an ionized reprocessor in NGC 6814 ». Astrophysical Journal 391 (mai 1992) : 102. http://dx.doi.org/10.1086/171327.

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26

Luo, Y. P., X. B. Zhang, C. Q. Luo, L. C. Deng et Z. Q. Luo. « Variable stars in the open cluster NGC 6811 ». New Astronomy 14, no 6 (août 2009) : 584–89. http://dx.doi.org/10.1016/j.newast.2009.02.005.

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27

Hyung, Siek, Lawrence H. Aller et Walter A. Feibelman. « Spectroscopic Observations of the Planetary Nebula NGC 6818 ». Astrophysical Journal 514, no 2 (avril 1999) : 878–94. http://dx.doi.org/10.1086/306970.

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28

Doroshenko, V. T. « UBV photometry of Seyfert galaxies. II. NGC 6814 ». Astrophysics 28, no 2 (1988) : 135–41. http://dx.doi.org/10.1007/bf01004059.

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29

Carraro, G., A. Buzzoni, E. Bertone et L. Buson. « UB CCD PHOTOMETRY OF THE OLD, METAL-RICH, OPEN CLUSTERS NGC 6791, NGC 6819, AND NGC 7142 ». Astronomical Journal 146, no 5 (11 octobre 2013) : 128. http://dx.doi.org/10.1088/0004-6256/146/5/128.

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30

Hyung, S., et L. H. Aller. « High dispersion spectra of Planetary Nebulae ». Symposium - International Astronomical Union 180 (1997) : 242. http://dx.doi.org/10.1017/s007418090013061x.

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Determinations of the plasma diagnostics and chemical compositions of planetary nebulae require ultimately high dispersion spectra. For objects of high surface brightness the Hamilton Echelle Spectrograph at Lick Observatory is satisfactory for the region 3650–10100Å which involves the 168th to 56th echelle orders. For a slit width of 640 μm amounting to 1.15 arcsec at the Coude focus, the actual spectral resolution (FWHM) is about 0.2Å at 8850Å. The length of the slit is chosen as 4.0 arcsec. Hyung (1994) & Aller (1994) describe the observing procedure. Since the Hamilton echelle was designed primarily for star-like sources, it is not useful for extended low surface brightness PN. The earlier observations were obtained with an 800 × 800 chip that did not cover the echelle field, so several settings were needed. Later, we used a slower 2048 × 2048 chip which covered the whole field and was somewhat more efficient at longer wavelengths. The program has been completed and definitive measurements have obtained for NGC 2440, NGC 6543, NGC 6741, NGC 6818, NGC 7026, NGC 7662, and Hu 1-2. All of these PN display particularly rich, interesting spectra. Previously observed and published objects include IC 351, IC 418, IC 2149, IC 4997, NGC 6567, NGC 6572, NGC 6790, NGC 6886, NGC 7009, BD +30 3639, & Hubble 12. NGC 6884 is in press. Additional nebulae which are yet to be discussed are IC 4634, IC 4846, IC 5117, NGC 6210, & NGC 6803.
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31

Anthony-Twarog, Barbara J., Constantine P. Deliyannis et Bruce A. Twarog. « AuvbyCaHβ ANALYSIS OF THE OLD OPEN CLUSTER, NGC 6819 ». Astronomical Journal 148, no 3 (7 août 2014) : 51. http://dx.doi.org/10.1088/0004-6256/148/3/51.

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32

Aarslev, Magnus J., Günter Houdek, Rasmus Handberg et Jørgen Christensen-Dalsgaard. « Modelling linewidths of Kepler red giants in NGC 6819 ». Monthly Notices of the Royal Astronomical Society 478, no 1 (30 mai 2018) : 69–80. http://dx.doi.org/10.1093/mnras/sty978.

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33

Done, C., G. M. Madejski, R. F. Mushotzky, T. J. Turner, K. Koyama et H. Kunieda. « The X-ray variability of NGC 6814 - Power spectrum ». Astrophysical Journal 400 (novembre 1992) : 138. http://dx.doi.org/10.1086/171979.

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34

Vio, R., R. Turolla, S. Cristiani et C. Barbieri. « A stochastic model for the variability of NGC 6814 ». Astrophysical Journal 405 (mars 1993) : 163. http://dx.doi.org/10.1086/172349.

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35

Jurua, Edward, Otto Trust et Felix Kampindi. « KIC 5110739 : A new Red Giant in NGC 6819 ». Proceedings of the International Astronomical Union 14, S343 (août 2018) : 434–35. http://dx.doi.org/10.1017/s1743921318007998.

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AbstractThe Kepler Input Catalogue (KIC) misclassified a number of red giant stars as sub giants. This could have resulted from the large uncertainties in the KIC surface gravities. This resulted in 1523 stars which were recently classified as red giant stars. The cluster membership of the 1523 red giant stars was determined using age, distance modulus, and variation of colour magnitude with large frequency separation. We found that one star, KIC 5110739, is a member of NGC 6819.
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36

Troyer, Jon, David Starkey, Edward M. Cackett, Misty C. Bentz, Michael R. Goad, Keith Horne et James E. Seals. « Correlated X-ray/ultraviolet/optical variability in NGC 6814 ». Monthly Notices of the Royal Astronomical Society 456, no 4 (14 janvier 2016) : 4040–50. http://dx.doi.org/10.1093/mnras/stv2862.

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37

Meibom, Søren, Sydney A. Barnes, David W. Latham, Natalie Batalha, William J. Borucki, David G. Koch, Gibor Basri et al. « THE KEPLER CLUSTER STUDY : STELLAR ROTATION IN NGC 6811 ». Astrophysical Journal 733, no 1 (2 mai 2011) : L9. http://dx.doi.org/10.1088/2041-8205/733/1/l9.

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38

Molenda-Żakowicz, J., K. Brogaard, E. Niemczura, M. Bergemann, A. Frasca, T. Arentoft et F. Grundahl. « Spectroscopic study of the open cluster NGC 6811★ ». Monthly Notices of the Royal Astronomical Society 445, no 3 (18 octobre 2014) : 2446–61. http://dx.doi.org/10.1093/mnras/stu1934.

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39

Bentz, Misty C., Laura Ferrarese, Christopher A. Onken, Bradley M. Peterson et Monica Valluri. « A Cepheid-based Distance to the Seyfert Galaxy NGC 6814 ». Astrophysical Journal 885, no 2 (12 novembre 2019) : 161. http://dx.doi.org/10.3847/1538-4357/ab48fb.

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40

Sekiguchi, K., et J. W. Menzies. « Spectral variations in the broad-line region of NGC 6814 ». Monthly Notices of the Royal Astronomical Society 245, no 1 (1 juillet 1990) : 66. http://dx.doi.org/10.1093/mnras/245.1.66.

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Summary We present optical spectroscopy of the Seyfert galaxy NGC 6814 obtained at the SAAO over a two-year period from 1983 May to 1985 October. During this period, the spectrum changed from Seyfert 1 to more closely resemble that of Seyfert 1.8-1.9. The Hβ flux decreased by more than a factor of 2 within two months. The decrease in the broad Balmer emission line strength was coupled with a decrease in the X-ray output.
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41

Knapen, Johan H., Nina Arnth-Jensen, Jordi Cepa et John E. Beckman. « Statistics and properties of H II regions in NGC 6814 ». Astronomical Journal 106 (juillet 1993) : 56. http://dx.doi.org/10.1086/116620.

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42

Street, R. A., Keith Horne, T. A. Lister, A. Penny, Y. Tsapras, A. Quirrenbach, N. Safizadeh, J. Cooke, D. Mitchell et A. Collier Cameron. « Variable stars in the field of open cluster NGC 6819 ». Monthly Notices of the Royal Astronomical Society 330, no 3 (mars 2002) : 737–54. http://dx.doi.org/10.1046/j.1365-8711.2002.05125.x.

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43

Yamauchi, M., M. Matsuoka, N. Kawai et A. Yoshida. « X-ray spectral structure of the Seyfert galaxy NGC 6814 ». Astrophysical Journal 395 (août 1992) : 453. http://dx.doi.org/10.1086/171664.

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44

Carlberg, Joleen K., Verne V. Smith, Katia Cunha, Steven R. Majewski, Szabolcs Mészáros, Matthew Shetrone, Carlos Allende Prieto et al. « THE PUZZLING Li-RICH RED GIANT ASSOCIATED WITH NGC 6819 ». Astrophysical Journal 802, no 1 (13 mars 2015) : 7. http://dx.doi.org/10.1088/0004-637x/802/1/7.

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45

Basu, Sarbani, Frank Grundahl, Dennis Stello, Thomas Kallinger, Saskia Hekker, Benoit Mosser, Rafael A. García et al. « SOUNDING OPEN CLUSTERS : ASTEROSEISMIC CONSTRAINTS FROM KEPLER ON THE PROPERTIES OF NGC 6791 AND NGC 6819 ». Astrophysical Journal 729, no 1 (9 février 2011) : L10. http://dx.doi.org/10.1088/2041-8205/729/1/l10.

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46

Duarte Puertas, S., J. Iglesias-Páramo, J. M. Vilchez, L. Drissen, C. Kehrig et T. Martin. « Searching for intergalactic star forming regions in Stephan’s Quintet with SITELLE ». Astronomy & ; Astrophysics 629 (septembre 2019) : A102. http://dx.doi.org/10.1051/0004-6361/201935686.

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Stephan’s Quintet (SQ), the prototypical compact group of galaxies in the local Universe, has been observed with the imaging Fourier transform spectrometer SITELLE, attached to the Canada-France-Hawaii-Telescope, to perform a deep search for intergalactic star-forming emission. In this paper we present the extended ionised gaseous structures detected and analyse their kinematical properties. The large field of view (11′ × 11′) and the spectral ranges of SITELLE have allowed a thorough study of the entire galaxy system, its interaction history and the main properties of the ionised gas. The observations have revealed complex three-dimensional strands in SQ seen for the first time, as well as the spatially resolved velocity field for a new SQ dwarf galaxy (M 82-like) and the detailed spectral map of NGC 7320c, confirming its AGN nature. A total of 175 SQ Hα emission regions have been found, 22 of which present line profiles with at least two kinematical components. We studied 12 zones and 28 sub-zones in the SQ system in order to define plausible physical spatial connections between its different parts in the light of the kinematical information gathered. In this respect we have found five velocity systems in SQ: (i) v = [5600−5900] km s−1 associated with the new intruder and the southern debris region; (ii) v = [5900−6100] km s−1, associated with the north starburst A and south starburst A and the strands connected to these zones; (iii) v = [6100−6600] km s−1, associated with the strands from the large-scale shock region (LSSR); (iv) v = [6600−6800] km s−1, associated with the young tidal tail, the starburst A (SQA), NGC 7319, and the NGC 7319 north lobe; and (v) v = [6800−7000] km s−1, associated with the strands seen connecting LSSR with SQA. We fail to detect ionised gas emission in the old tail, neither in the vicinity of NGC 7318A nor in NGC 7317, and the connection between NGC 7319 north lobe and SQA cannot be confirmed. Conversely, a clear gaseous bridge has been confirmed both spatially and kinematically between the LSSR zone and the NGC 7319 AGN nucleus. Finally, a larger scale, outer rim winding the NGC 7318B/A system clockwise north-west to south-east has been highlighted in continuum and in Hα. This structure may be reminiscent of a sequence of a previously proposed scenario for SQ a sequence of individual interactions.
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47

Wu, T., Y. Li et S. Hekker. « ASTEROSEISMIC STUDY ON CLUSTER DISTANCE MODULI FOR RED GIANT BRANCH STARS IN NGC 6791 AND NGC 6819 ». Astrophysical Journal 786, no 1 (9 avril 2014) : 10. http://dx.doi.org/10.1088/0004-637x/786/1/10.

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48

Velloso, E. N., J. D. do Nascimento, Jr. et S. H. Saar. « Long-term Periodicities in Kepler Photometry of Open Cluster NGC 6811 ». Astrophysical Journal 900, no 2 (14 septembre 2020) : 173. http://dx.doi.org/10.3847/1538-4357/aba8a3.

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49

Campana, Sergio, et Luigi Stella. « An estimate of the central black hole mass in NGC 6814 ». Monthly Notices of the Royal Astronomical Society 264, no 2 (septembre 1993) : 395–401. http://dx.doi.org/10.1093/mnras/264.2.395.

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Platais, Imants, Natalie M. Gosnell, Søren Meibom, Vera Kozhurina-Platais, Andrea Bellini, Christian Veillet et Martin S. Burkhead. « WIYN OPEN CLUSTER STUDY. LV. ASTROMETRY AND MEMBERSHIP IN NGC 6819 ». Astronomical Journal 146, no 2 (16 juillet 2013) : 43. http://dx.doi.org/10.1088/0004-6256/146/2/43.

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