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Al di la della Luna; Beyond the Moon; Astrophotography; Astrofotografia; Danilo Pivato
 
 
 
 
 
 
 
The Analysis of Frame
 

M 3; NGC 5272; GCL 25; h 1663; CG 3636; C 1339+286: Globular Cluster - [field: 0,34° x 0,68°] - Mag. Limite: 20.7^ (r) - Fonte: SDSS DR12 - Object Coordinates: RAJ2000.0 13h 42m 11.62s - Dec J2000.0 +28° 22' 38.2" [SIMBAD] - Magnitudine: 6.35^ (v); --.-^ (b); Surface Brightness: --.-^ - Object Size: 18' - Position Angle: --° - Object Classification: 6; Redshift z(~): -0.000471 - Spectrum: ---. Ammasso globulare tra i più belli della sua categoria. A questa scala immagine (1,107"/pixel) si presenta luminoso ed imponente tanto da occupare quasi tutto il campo. La stella più luminosa è la SAO 82956 di magnitudine 9,0v. Nel campo rientrano due stelle di 10^ mag e quattro poco superiori all'11^v. I 300 secondi di posa di esposizione a f/5 hanno appena appena contribuito alla formazione del blooming delle stelle più luminose presenti nella parte centrale del globulare. M3 è stata la prima scoperta originale di Charles Messier avvenuta nel 1764 e, a quanto sembra, fu proprio la scoperta di questo oggetto, a suggerire a Charles Messier la necessità di non lasciare al caso, come già per M1 ed M2, la scoperta di questi oggetti simili a comete, ma bensì di dare inizio ad una ricerca sistematica. All'epoca della scoperta Messier descrisse M3 come: "Nebulosa scoperta tra Bootes ed uno dei Cani da Caccia di Hevelius; essa non contiene alcuna stella, il suo centro è brillante e la sua luce va scemando insensibilmente, essa è rotonda; con un bel cielo la si può vedere con un telescopio da un piede; essa è riportata sulla carta della cometa osservata nel 1779. Memorie dell'Accademia dello stesso anno. Riosservata il 29 marzo 1781, sempre bellissima." . Secondo le ultime stime l'ammasso globulare è formato da circa 500.000 stelle e dista da noi 34.000 anni luce. Le stelle più brillanti dell'ammasso giungono appena alla 12.5^ (v) magnitudine. William Herschel fu il primo a constatarne la nautra di agglomerato stellare, grazie all'impiego del suo potente riflettore. Lord Rosse riuscì a scorgere nel suo interno delle strutture filiformi alternate a zone buie come in M13. In M3 fino ad oggi sono state scoperte 274 variabili, di gran lunga il più alto numero riscontrato in qualsiasi ammasso globulare. 133 sono del tipo RR Lyrae.

 
 
 
Description of the other deep-sky object in the filed:
 
 
 
 

 

 
Historical observations and descriptions:
 

Charles Messier: May 3, 1764. 3. 13h 31m 25s (202d 51' 19") +29d 32' 57" - Nebula discovered between Bootes & one of the Hunting Dogs of Hevelius [Canes Venatici], it doesn't contain any star, its center is brilliant, & its light is gradually fading away, it is round; in a beautiful [dark] sky, one can see it in a telescope of 1-foot [FL]: It is reported on the chart of the comet observed in 1779. Memoirs of the Academy of the same year. Reviewed on March 29, 1781, always very beautiful. (Diam. 3')

[Handwritten remark in Messier's copy:] Reviewed on January 9, 1790.

[Mem. Acad. for 1771, p. 437 (first Messier catalog)]
On May 3, 1764, when working on a catalog of the nebulae, I have discovered one between Bootes & one of the Hunting Dogs [Canes Venatici] of Hevelius, the southernmore of the two, exactly between the tail & the paws of this Dog, according to the charts of Flamsteed. I have observed that nebula on the meridian, & I compared with Mu Bootis; its right ascension has been found as 202d 51' 19", & its declination as 29d 32' 57" north. That nebula which I have examined with a Gregorian telescope of 30 pouces focal length, which magnifies 104 times, doesn't contain any star; the center is brilliant, & the light gets lost fading [outward]; it is round, & could have 3 minutes of arc in diameter. One can see it in a good sky with an ordinary [nonachromatic] refractor of one foot [FL]. - [p. 454] 1764.May. 3. RA: 202.51.19, Dec: 29.32.57.B, Diam: 0. 3. Nebula without stars, between the tail & the legs of one of the Hunting Dogs of Hevelius.

 
Johann Gottfried Koehler: [Letter to J.E. Bode of June 17, 1782] Some days ago I have discovered a nebulous star not included in your catalog [Bode's catalog] near the 3rd and 9th star of Bootes, with that stars if makes an almost equilateral triangle. It has the following position [..], RA 203d 4' 0" [13h 32m 16s], Dec +29d 24' 45", [and is of] rather vivid magnitude.
 
Johan Elert Bode: - (1782) Canes Venatici 48. - [From: Vorstellung der Gestirne auf XXXIV Kupfertafeln (Introduction to the Stars on 34 Copper Plates), 1782. P. 8, plate 7] - CVn 48, after Messier. RA: 203:03 [13:32.2], Dec: +26:28. Nebulous patch.
 
William Herschel: - [1784. PT Vol. LXXIV=74 (1784), p. 437-451, here p. 440] .. To these may added the 1st, 3d [M3], 27, 33, 57, 79, 81, 82, 101 [of Messier's catalog], which in my 7, 10, and 20-feet reflectors shewed a mottled kind of nebulosity, which I shall call resolvable; so that I expect my present telescope will, perhaps, render the stars visible of which I suppose them to be composed. ..

[PT 1814, p. 276, SP2 p. 536] Sept. 24, 1810. Large 10 feet Newtonian telescope. Space penetrating power 75.82. Magnifying powers 71, 108, 171, 220. "The 3rd of the Connoiss. [M3, NGC 5272] is one of the globular clusters; very brilliant and beautiful. The compression of the stars begins to increase pretty suddenly from the outside at 3/4 of the radius, and continues gradually up to its centre, its diameter taking in the outside is full half of the field of the glass magnifying 171 times, giving 4'30"."

[PT 1818, p. 436, SP2 p. 595]
The 3rd of the Connoissance.
"1813, 7 feet finder of the telescope. It is at a small distance from a star of equal brightness ; the star is clear, the object is hazy, and somewhat larger than the star."
"1783, 7 feet telescope. With 460 the light is so feeble that the object can hardly be seen; I suspect some stars in it. 1813, with 80, many stars are visible in it."
"1799, 10 feet telescope, power 120; with an aperture of 4 inches it is resolvable; with 5 easily resolvable; with 6 it is resolvable; with 7 and all open the stars may be easily perceived."
"1784, 1785, 20 feet telescope. A beautiful cluster of stars, about 5 or 6 minutes in diameter."
"1810, Large 10 feet telescope. With 171 the diameter is full 4'30". (*)" (*) see above observation from [WH 1814].
By the observation of the 7 feet telescope this cluster must be of the 243rd order.

 

John Herschel - 1833 - h 1663 -

h 1663 = M3.
Sweep 417 (April 20, 1832).
RA 13h 34m 12.2s, NPD 60d 46' 22" (1830.0) [Right Ascension and North Polar Distance]
A most superb object, diam = 10s.0 time in RA. Not less than 1000 stars 11m and under. They run into a blaze at the centre, and form as it were radiating lines and pointed projections from the mass, with many stragglers.

Sweep 64 (March 26, 1827).
RA 13h 34m 18.0s, NPD 60d 45' 51" (1830.0)
I just see the stars through a cloud so thick as almost to obscure Arcturus; 6' diam, but in a clear night no doubt more.

Sweep 415 (April 17, 1832). RA 13h 34m 18.1s, NPD 60d 46' 8" (1830.0)
Observed with Capt. Smyth, who "saw something remarkable" in a small * 2m or 3m preceding it, which proved on closer examination to be a fine first class double *.

Sweep 65 (March 30, 1827). RA 13h 34m 19.5s, NPD 60d 45' 46" (1830.0)
Very beautiful; stars 11 .... 15m; fills field, making lines and irregular rays of stars, and coming up to a blaze in the middle.

Sweep 343 (April 13, 1831). RA 13h 34m 20.7s, NPD 60d 45' 38" (1830.0)
A noble globular cluster 5 or 6' diam, entirely resolved when not a star near it, even Arcturus, was visible to the naked eye for clouds.

 

William Henry Smyth: CCCCXCII [492]. M3

CCCCXCII. 3 M. Canum Venaticorum.
AR 13h 34m 45s, Dec N 29d 10'.6
Mean Epoch of Observation: 1831.26 [Apr 1831]
[with drawing]
A brilliant and beautiful globular congregation of not less than 1000 small stars, between the southern Hound and the knee of Boötes; it blazes splendidly towards the centre, and has outliers in all directions, except the sf [south following; SE], where it is so compressed that, with its stragglers, it has something of the figure of the luminous oceanic creature called Medusa pellucens. This noble object is situated in a triangle formed by three small stars in the np [north preceding; NW], nf [north following; NE], and sf [south following, SE] quadrabts, which, by their comparative brightness, add to the beauty of the field. It is nearly in mid-distance between Arcturus and Cor Caroli, at 11deg north-west of the former star. brp> This mass is one of those balls of compact and wedged stars, whose laws of aggregation it is so impossible to assign; but the rotundity of figure gives full indication of some general attractive bond of union. It was discovered in 1764 by Messier, who described it as "a nebula without a star, brilliant and round:" his instrument must have been rather moderate not to resolve this object, and it is matter of regret, that the exertions of such a man were straitened to such means. It was next pronounced to be a "mottled nebulosity;" but in 1784, Sir W. Herschel attacked it with his 20-foot reflector, and resolved it into a "beautiful cluster of stars, about 5' or 6' in diameter." By the gauging process, which he has fully described, he estimated its profundity to be of the 243rd order.

 

John Herschel, General Catalogue: GC 3636.

GC 3636 = h 1663 = M3.
RA 13h 35m 40.8s, NPD 60d 55' 6.0" (1860.0) [Right Ascension and North Polar Distance]
!!; Glob. Cl.; eB; vL; vsmbM; st 11 ... 14 observations by W. & J. Herschel.
Very remarkable; globular cluster; extremely bright; very large; very suddenly much brighter toward the middle; stars of 11th magnitude and fainter.

 

William Huggins:

[Further Observations on the Spectra of some Nebulae, with a Mode of determining the Brightness of these Bodies. Phil. Trans. Roy. Soc., Vol. 156 (1866), p. 381-397; here p. 389]
[No. [GC] 3636. 1663 h. 3 M. R.A. 13h 35m 40s. N.P.D. 60d 55' 6". Cluster; extremely bright.]
"Ein leicht auflöslicher Hauf zahlloser Sterne, in der Mitte zu einem einzigen Lichte von grosser Helligkeit zusammenlaufend." [An easily resolvable cluster of innummerable stars, converging to a single light of great brightness in the middle.] - D'Arrest
Spectrum continuous

 

John Louis Emil Dreyer: NGC 5272 -

NGC 5272 = GC 3636 = h 1663; M 3.
RA 13h 35m 44s, NPD 60d 54.9' (1860.0) [Right Ascension and North Polar Distance]
!!, Glob. Cl., eB, vL, vsmbM, st 11 ...; = M3
Very remarkable, globular cluster, extremely bright, very large, very suddenly much brighter toward the middle, stars of 11th magnitude and fainter.

 

Heber Doust Curtis:

[Descriptions of 762 Nebulae and Clusters photographed with the Crossley Reflector. Publ. Lick Obs., No. 13, Part I, p. 9-42]
NGC 5272, RA=13:37.6, Dec=+28:53. [Publ. Lick Obs.] Vol. VIII, Plate 48. M. 3. The main portion of this beautiful cluster is about 8' in diameter. 1 s.n.

 
Camille Flammarion: Les Etoiles et les Curiosites du Ciel - pagg. 125-126: "... La règion du ciel que nous décrivons en ce moment, celle qui est occupée par les Chiens de Chasse, la Grande Ourse, le Petit Lion, le Lion, la Chevelure de Bérénice, la Vierge, est la plus riche du ciel en nebuleuses. Non loin de la nebuleuse precedente [ndr: M51], dans la meme constellation, entre le Coeur de Charles et Arcturus, plutot plus pres de cette derniere etoile que de la premiere, on en voit une autre, moins belle assurement, mais neanmoins fort interessante, car c'est là un amas d'etoiles presque globulaire, de 6 a 7 minutes de diametre, et qui se montre composé d'environ un millier de soleils (fig. 83).Trois etoiles relativement brillantes semblent l'enfermar dans un triangle et ajoutent encore à la beautè du champ. Voilà encore un univers lointain qui s'offre à nos regards à travers les profounders de l'immensité. Cet amas d'étoiles devient magnifique (fig.84), vu dans une lunette de quinze ou seize centrimetes; deux soleils etincellent au centre, et plusieurs trainées d'étoiles semblent rayonner au loin, comme si la gravitation les avait disposées en lignes symetriques. Quel poeme que cet univers perdu au fond des cieux! Qu'il est plus eloquent à lui seul que l'Iliade, l'Odyssée, la Divine Comédie, la Jèrusalem delivrée et la Henriade réunies!..."
 
Burnham's Celestial Handbook - Vol. 1 pag. 362 - 367; 3 photograps and 1 diagram: " ... A beautiful bright globular star cluster, one of the most splendid in the sky. (... Continue)
 
 
 
Variable Stars in Globular cluster M3 (NGC 5272) show in the map - Interactive Table - (by Benko+, 2006 )
 
 
SIMBAD Name Full Seq m Periodo d Type BMag VMag IMag FileName SIMBAD NAme RA deg Dec deg
 
Cl* NGC 5272 SAW V 1
1
 
0.520596300   RRab 15.900   15.631   15.227   v001 Cl* NGC 5272 SAW V 1 205.54663 +28.34268
Cl* NGC 5272 SAW V 5
5
 
0.505703000   RRab 15.974   15.714   15.238 : v005 Cl* NGC 5272 SAW V 5 205.63067 +28.37237
Cl* NGC 5272 SAW V 6
6
 
0.514332700   RRab 16.003   15.703   15.276   v006 Cl* NGC 5272 SAW V 6 205.50937 +28.39497
Cl* NGC 5272 SAW V 9
9
 
0.541555300   RRab 15.957   15.645   15.217   v009 Cl* NGC 5272 SAW V 9 205.45662 +28.32025
Cl* NGC 5272 SAW V 10
10
 
0.569546500   RRab 16.004   15.647   15.152   v010 Cl* NGC 5272 SAW V 10 205.59655 +28.41677
Cl* NGC 5272 SAW V 11
11
 
0.507891500   RRab 15.873   15.636   15.166   v011 Cl* NGC 5272 SAW V 11 205.50035 +28.31999
Cl* NGC 5272 SAW V 12
12
 
0.317934700   RRc 15.814   15.606   15.275   v012 Cl* NGC 5272 SAW V 12 205.54722 +28.33808
Cl* NGC 5272 SAW V 13
13
 
0.479504300   RRd 15.917   15.684   15.239   v013 Cl* NGC 5272 SAW V 13 205.54029 +28.33954
Cl* NGC 5272 SAW V 14
14
 
0.635900200   RRab 15.867   15.551   15.050   v014 Cl* NGC 5272 SAW V 14 205.53295 +28.33369
Cl* NGC 5272 SAW V 15
15
 
0.530087400   RRab 15.833   15.616   15.144   v015 Cl* NGC 5272 SAW V 15 205.51984 +28.30237
Cl* NGC 5272 SAW V 16
16
 
0.511494300   RRab 16.020   15.701   15.288   v016 Cl* NGC 5272 SAW V 16 205.45331 +28.35226
Cl* NGC 5272 SAW V 18
18
 
0.516452700   RRab 16.068 : 15.698   15.231 : v018 Cl* NGC 5272 SAW V 18 205.57928 +28.29646
Cl* NGC 5272 SAW V 21
21
 
0.515758000   RRab 16.012   15.690       v021 Cl* NGC 5272 SAW V 21 205.65780 +28.38375
Cl* NGC 5272 SAW V 22
22
 
0.481420500   RRab 15.989 : 15.698   15.269   v022 Cl* NGC 5272 SAW V 22 205.60832 +28.37548
Cl* NGC 5272 SAW V 23
23
 
0.595383400   RRab 15.884   15.639   14.677   v023 Cl* NGC 5272 SAW V 23 205.51220 +28.45566
Cl* NGC 5272 SAW V 24
24
 
0.663380000   RRab 15.914   15.533   15.060   v024 Cl* NGC 5272 SAW V 24 205.50172 +28.38105
Cl* NGC 5272 SAW V 26
26
 
0.597742700   RRab 15.891   15.596   14.991   v026 Cl* NGC 5272 SAW V 26 205.49260 +28.36621
Cl* NGC 5272 SAW V 34
34
 
0.559103100   RRab 16.067   15.768   15.177   v034 Cl* NGC 5272 SAW V 34 205.59082 +28.42569
Cl* NGC 5272 SAW V 35
35
 
0.530548300   RRab 15.878   15.620   15.112 : v035 Cl* NGC 5272 SAW V 35 205.51475 +28.30100
Cl* NGC 5272 SAW V 36
36
 
0.545592900   RRab 15.854   15.601   15.214   v036 Cl* NGC 5272 SAW V 36 205.60267 +28.36868
Cl* NGC 5272 SAW V 37
37
 
0.326637800   RRc 15.903   15.679   15.302   v037 Cl* NGC 5272 SAW V 37 205.47349 +28.42339
Cl* NGC 5272 SAW V 38
38
 
0.558011000   RRab 16.086   15.701   15.171   v038 Cl* NGC 5272 SAW V 38 205.48382 +28.41360
Cl* NGC 5272 SAW V 39
39
 
0.587075800   RRab 16.021   15.668   15.206   v039 Cl* NGC 5272 SAW V 39 205.47110 +28.41173
Cl* NGC 5272 SAW V 40
40
 
0.551539400   RRab 16.038   15.672   15.218   v040 Cl* NGC 5272 SAW V 40 205.46256 +28.40915
Cl* NGC 5272 SAW V 41
41
 
0.485877700   RRab 16.001   15.659   15.292   v041 Cl* NGC 5272 SAW V 41 205.51862 +28.39321
Cl* NGC 5272 SAW V 44
44
 
0.506380100   RRab 15.912   15.615   15.160   v044 Cl* NGC 5272 SAW V 44 205.60225 +28.40626
Cl* NGC 5272 SAW V 45
45
 
0.536900200   RRab 16.056   15.675   15.247   v045 Cl* NGC 5272 SAW V 45 205.47215 +28.34165
Cl* NGC 5272 SAW V 46
46
 
0.613383200   RRab 16.028   15.703   15.153   v046 Cl* NGC 5272 SAW V 46 205.50791 +28.36402
Cl* NGC 5272 SAW V 47
47
 
0.540912800   RRab 15.941   15.648   15.190   v047 Cl* NGC 5272 SAW V 47 205.51125 +28.35799
Cl* NGC 5272 SAW V 48
48
 
0.627829900   RRab 15.922   15.615       v048 Cl* NGC 5272 SAW V 48 205.58855 +28.35033
Cl* NGC 5272 SAW V 49
49
 
0.548204800   RRab     15.645       v049 Cl* NGC 5272 SAW V 49 205.59242 +28.35067
Cl* NGC 5272 SAW V 50
50
 
0.512839200   RRab 15.991   15.645   15.165   v050 Cl* NGC 5272 SAW V 50 205.55137 +28.31332
Cl* NGC 5272 SAW V 51
51
 
0.583970200   RRab 16.041   15.658   15.187 : v051 Cl* NGC 5272 SAW V 51 205.55822 +28.31556
Cl* NGC 5272 SAW V 52
52
 
0.516229900   RRab     15.756       v052 Cl* NGC 5272 SAW V 52 205.52381 +28.42036
Cl* NGC 5272 SAW V 55
55
 
0.529820700   RRab 15.976   15.673       v055 Cl* NGC 5272 SAW V 55 205.48365 +28.46825
Cl* NGC 5272 SAW V 56
56
0.329600000 RRc 15.866 15.642 15.253 v056 Cl* NGC 5272 SAW V 56 205.50311 +28.47767
Cl* NGC 5272 SAW V 57
57
 
0.512188500   RRab 16.001   15.699   15.357   v057 Cl* NGC 5272 SAW V 57 205.59768 +28.37841
Cl* NGC 5272 SAW V 59
59
 
0.588823600   RRab 16.071   15.649   15.170   v059 Cl* NGC 5272 SAW V 59 205.51384 +28.31481
Cl* NGC 5272 SAW V 60
60
 
0.707728000   RRab 15.936   15.506       v060 Cl* NGC 5272 SAW V 60 205.45474 +28.29042
Cl* NGC 5272 SAW V 62
62
 
0.652409900   RRab 16.027   15.643   15.085   v062 Cl* NGC 5272 SAW V 62 205.57627 +28.49424
Cl* NGC 5272 SAW V 63
63
 
0.570400400   RRab 16.052   15.670   15.163   v063 Cl* NGC 5272 SAW V 63 205.55966 +28.47331
Cl* NGC 5272 SAW V 64
64
 
0.605458800   RRab 16.045   15.672   15.156 : v064 Cl* NGC 5272 SAW V 64 205.58414 +28.47009
Cl* NGC 5272 SAW V 65
65
 
0.668347400   RRab 15.875   15.497   14.991   v065 Cl* NGC 5272 SAW V 65 205.58752 +28.46945
Cl* NGC 5272 SAW V 66
66
 
0.620180700   RRab 15.991   15.641   15.142   v066 Cl* NGC 5272 SAW V 66 205.51612 +28.41169
Cl* NGC 5272 SAW V 68
68
 
0.355991100   RRd 15.916   15.632   15.265   v068 Cl* NGC 5272 SAW V 68 205.55490 +28.42700
Cl* NGC 5272 SAW V 70
70
 
0.486351800   RRc(?) 15.670   15.386   14.953   v070 Cl* NGC 5272 SAW V 70 205.56004 +28.42065
Cl* NGC 5272 SAW V 71
71
 
0.549053000   RRab 16.008   15.796   15.024   v071 Cl* NGC 5272 SAW V 71 205.59936 +28.37793
Cl* NGC 5272 SAW V 72
72
 
0.456078000   RRab 15.953   15.670   15.320   v072 Cl* NGC 5272 SAW V 72 205.68881 +28.37817
Cl* NGC 5272 SAW V 73
73
 
0.673611000   RRab 16.047   15.626   15.092   v073 Cl* NGC 5272 SAW V 73 205.68664 +28.39600
Cl* NGC 5272 SAW V 75
75
 
0.314076700   RRc 15.890   15.626   15.319   v075 Cl* NGC 5272 SAW V 75 205.56385 +28.42281
Cl* NGC 5272 SAW V 79
79
 
0.358072700   RRd 15.988   15.742   15.266   v079 Cl* NGC 5272 SAW V 79 205.56164 +28.47541
Cl* NGC 5272 SAW V 80
80
 
0.538378800   RRab 15.955   15.632   15.205   v080 Cl* NGC 5272 SAW V 80 205.67965 +28.45771
Cl* NGC 5272 SAW V 83
83
 
0.501263100   RRab 15.960 : 15.674   15.228 : v083 Cl* NGC 5272 SAW V 83 205.40870 +28.40924
Cl* NGC 5272 SAW V 84
84
 
0.595728900   RRab 16.042   15.658   15.158   v084 Cl* NGC 5272 SAW V 84 205.56835 +28.42423
Cl* NGC 5272 SAW V 85
85
 
0.355819100   RRc 15.754   15.574   15.176   v085 Cl* NGC 5272 SAW V 85 205.64469 +28.44139
Cl* NGC 5272 SAW V 90
90
 
0.517030800   RRab 16.008 : 15.673   15.190 : v090 Cl* NGC 5272 SAW V 90 205.57920 +28.32612
Cl* NGC 5272 SAW V 93
93
 
0.602296000   RRab 16.021   15.640   15.143   v093 Cl* NGC 5272 SAW V 93 205.44790 +28.26784
Cl* NGC 5272 SAW V 96
96
 
0.499415000   RRab 15.918   15.652       v096 Cl* NGC 5272 SAW V 96 205.49670 +28.31321
Cl* NGC 5272 SAW V 97
97
 
0.334932600   RRc 15.933   15.703   15.355   v097 Cl* NGC 5272 SAW V 97 205.50742 +28.32356
Cl* NGC 5272 SAW V 99
99
 
0.360931900   RRd 15.824 : 15.590   15.096 : v099 Cl* NGC 5272 SAW V 99 205.61180 +28.36325
Cl* NGC 5272 SAW V105
105
 
0.287744000   RRc 15.791   15.580   15.306   v105 Cl* NGC 5272 SAW V105 205.54138 +28.43147
Cl* NGC 5272 SAW V106
106
 
0.547131600   RRab 16.039   15.675   15.223   v106 Cl* NGC 5272 SAW V106 205.53287 +28.42491
Cl* NGC 5272 SAW V108
108
 
0.519610000   RRab 16.000   15.708   15.241   v108 Cl* NGC 5272 SAW V108 205.47857 +28.46447
Cl* NGC 5272 SAW V118
118
 
0.499390500   RRab 15.987   15.672       v118 Cl* NGC 5272 SAW V118 205.59413 +28.29734
Cl* NGC 5272 SAW V119
119
 
0.517690000   RRab 15.966 : 15.670   15.182 : v119 Cl* NGC 5272 SAW V119 205.62850 +28.40811
Cl* NGC 5272 SAW V120
120
 
0.640140000   RRab 16.007   15.628   15.090   v120 Cl* NGC 5272 SAW V120 205.45442 +28.44223
Cl* NGC 5272 SAW V124
124
 
0.752439000   RRab 16.000   15.544   14.942   v124 Cl* NGC 5272 SAW V124 205.52755 +28.32239
Cl* NGC 5272 SAW V125
125
 
0.349822700   RRc 15.959   15.730   15.220   v125 Cl* NGC 5272 SAW V125 205.60722 +28.34171
Cl* NGC 5272 SAW V126
126
 
0.348406200   RRc 15.887   15.622   15.271   v126 Cl* NGC 5272 SAW V126 205.54350 +28.33769
Cl* NGC 5272 SAW V202
202
 
0.773571000   RRab 15.959   15.558   14.977 : v202 Cl* NGC 5272 SAW V202 205.42883 +28.40481
Cl* NGC 5272 SAW V203
203
 
0.289794000   RRc 15.855   15.592   15.252   v203 Cl* NGC 5272 SAW V203 205.53972 +28.29174
Cl* NGC 5272 SAW V222
222
 
0.596744600   RRab 15.931   15.572   15.042   v222 Cl* NGC 5272 SAW V222 205.57899 +28.36084
Cl* NGC 5272 SAW V236
236
 
  ? long             v236 Cl* NGC 5272 SAW V236 205.67323 +28.31891
Cl* NGC 5272 SAW V260
260
 
  ? long             v260 Cl* NGC 5272 SAW V260 205.49319 +28.26461
                                 
                                 
                                 
                                 
 

Abstract:

We present time-series data on the variable stars of the galactic globular cluster Messier 3 (M3). We give BVIC light curves for 74 RR Lyrae, along with estimated fundamental photometric parameters such as intensity and magnitude-averaged brightness and pulsation periods. In some cases, the periods we have found significantly differ from the previously published ones. The I-band light curve has not been observed previously for numerous (74 variables. Three new RR Lyrae variables have been discovered. Groups of RR Lyrae variables that belong to different evolutionary stages and have been separated previously on the basis of V data were found here for all colours and colour indices by cluster analysis. The I-band period-luminosity relation is also discussed. From the 66 modulated (Blazhko type) RR Lyrae stars we investigated, six are newly identified and two of them are first overtone pulsators. In the case of 13 RR Lyrae, the period of Blazhko cycle has been estimated for the first time. Amplitude ratios of RRd stars have been investigated to search possible mode content changes. In contrast to previous publications no changes have been found. Problems with the sampling of the time-series of typical cluster variability surveys are demonstrated. Description: The observational material of M3 was obtained in two seasons (1998 and 1999) with two telescopes. Both telescopes are mounted at Piszkestet Mountain Station of the Konkoly Observatory. You click on the white lettering.

 
 
       
 
Since: 01/01/2004
 
       
 
Since: 01/11/2010