Weekly Information about Bright Comets (2006 Mar. 11: North)

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Updated on March 17, 2006
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Best time and the azimuth, altitude (A,h) are at lat. 35 deg in the Northern Hemisphere.

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* C/2006 A1 ( Pojmanski )

New comet discovered in early January by the southern survey ASAS. It brightened rapidly and reached to 5.2 mag at best in late February and early March. Now it is still bright as 5.6 mag (Mar. 10, Katsumi Yoshimoto). Very strongly condensed, and rather small considering its brightness, with a diameter of several arcmins. Long tail is also visible. It became unobservable in the Southern Hemisphere. In the Northern Hemisphere, it keeps observable in good condition until it fades out. It will be fading gradually in the morning sky after this. It will be visible visually until May.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  20 54.69   17  5.9   0.806   0.674    42    6.0   4:53 (266, 24)  
Mar. 18  21 24.66   31 39.7   0.905   0.769    47    6.8   4:43 (250, 29)  

* C/2005 E2 ( McNaught )

It has been visible visually in the southern low sky since last August. It has been bright as 10 mag for three months since December. It was very small and sharp before, however, now it looks like a typical diffuse comet. The altitude is getting lower slowly in the evening sky, and it will be too low to observe in April. It will appear in the morning sky again in late August at 13.5 mag. It will come to locate high in October, then it will be visible visually again at 14 mag.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   0 57.24   15 35.1   2.310   1.535    30   10.1  19:27 (101, 12)  
Mar. 18   1 18.77   18 20.5   2.341   1.552    29   10.2  19:33 (105, 11)  

* 73P-C/Schwassmann-Wachmann 3

It will pass only 0.08 A.U. from the earth on May 12, remarkable approach after 76 years since its discovery in 1930. It was expected be so bright as 2 mag, but actually, it was fainter than its last appearance by 1.5 mag. Anyway, it will be 3.5 mag at best, and will be visible with naked eyes. It is already bright and visible visually, 11.9 mag on Mar. 10 (Katsumi Yoshimoto). Strongly condensed and easy to see. It keeps observable in good condition all through the encounter in May, while it will be brightening rapidly. Two other components B and G are also bright. The components B and G are fainter than the main component by 2.5 mag and 5.5 mag respectively. Due to the approach of the comet, Bootids meteor shower observed in 1930 may appear in outburst again in May and June. But the earth will not pass through the dust trail in calculation.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  14 10.67   14 33.0   0.635   1.523   137   11.3   2:57 (  0, 69)  
Mar. 18  14 20.03   15 58.6   0.547   1.457   140   10.6   2:39 (  0, 71)  

* C/2004 B1 ( LINEAR )

It was expected to reach to 9 mag in 2006 spring. But actually, the brightness evolution had been much slower than expected, 13.9 mag on Aug. 1 and 11.7 mag still on Oct. 27 (Michael Mattiazzo). Then, it has already started fading before the perihelion passage, 13.3 mag on Dec. 9 (Andrew Pearce). It had been too low even in the Southern Hemisphere from January to February, however, it will be getting higher gradually after this. Finally, it is getting observable in the morning sky also in the Northern Hemisphere. It will be observable in good condition after this until autumn. Now it is 12.0 mag (Mar. 10, Terry Lovejoy). It may be visible bright as 12 mag until June.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  20 32.03  -26 53.7   2.166   1.657    47   12.0   4:53 (305,  2)  
Mar. 18  20 30.43  -24  6.3   2.076   1.683    53   12.0   4:43 (306,  7)  

* 73P-B/Schwassmann-Wachmann 3

One of the split components born in outburst in 1995. It is brighter than its last appearance in 2001 by 1 mag. It has been brightening as rapidly as the main component, and it is already visible visually. Now it is 13.8 mag (Mar. 5, Seiichi Yoshida). It will pass only 0.067 A.U. from the earth on May 14, remarkable approach after 76 years since its discovery in 1930. It is fainter than the main component by 2.5 mag, but will be closer to the earth than the main component. It will reach to 5.5 mag, and double naked eye comets will be visible. It keeps observable in good condition all through the encounter in May.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  14  5.16   15 11.9   0.639   1.533   138   13.9   2:52 (  0, 70)  
Mar. 18  14 13.39   16 43.2   0.551   1.467   141   13.2   2:32 (  0, 72)  

* C/2003 WT42 ( LINEAR )

It brightened faster than a typical comet, and became visible visually as 13.5 mag in October (Oct. 24, Seiichi Yoshida). Now it is still bright as 13.4 mag (Feb. 27, Seiichi Yoshida). Small and strongly condensed. Because it is distant from the sun, it keeps observable at 13.5 mag in good condition for a long time until 2006 June.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   9 43.49   52 50.7   4.540   5.196   126   13.5  22:27 (180, 72)  
Mar. 18   9 41.08   52 25.6   4.596   5.194   122   13.5  21:57 (180, 73)  

* 29P/Schwassmann-Wachmann 1

In 2005, outbursts occured in September and November, when it brightened up to 12.5-13 mag. It had been faint as around 15 mag in December and January. However, it has been bright at around 13 mag since late January. It was still bright as 12.5 mag on Feb. 22 (Juan Jose Gonzalez). But it will be too low to observe in late March.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   2 13.17   22 23.3   6.397   5.793    48   13.8  19:27 ( 97, 31)  
Mar. 18   2 18.20   22 40.9   6.479   5.795    43   13.8  19:33 (101, 25)  

* 71P/Clark

It has been brightening as 18.2 mag on Dec. 24 (Ken-ichi Kadota), 16.2 mag on Feb. 4 (Katsumi Yoshimoto). But it is a bit fainter than originally predicted by 0.7 mag. It is getting brighter rapidly in the morning sky. It will become visible visually at 13 mag in April, and will reach to 12 mag in June. The condition is best beucase it is almost at opposition at the perihelion passage. However, it will be very low, only 13-20 deg high, from June to September in the Northern Hemisphere. When it gets higher again, it will be fainter than 14 mag, too faint to see visually.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  16 47.57  -17 53.3   1.344   1.771    97   14.8   4:53 (348, 36)  
Mar. 18  17  2.94  -18 48.7   1.257   1.742   100   14.5   4:43 (349, 35)  

* P/2005 XA54 ( LONEOS-Hill )

It was so faint as 18.5 mag at the discovery in early December, but it brightened up to 17 mag in mid January. Then it started brightening extremely rapidly after mid January. It was visible visually as bright as 14.0 mag in late February (Feb. 27, Seiichi Yoshida). Very strongly condensed and almost stellar. It will be observable in good condition at 14 mag until March. However, it will fade out soon after April.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  10 19.49   21 48.1   0.823   1.778   156   14.8  23:03 (  0, 77)  
Mar. 18  10 22.42   23 33.7   0.852   1.781   149   14.9  22:39 (  0, 79)  

* C/2005 B1 ( Christensen )

It will pass the perihelion soon, in 2006 February. But it did not brightened so much as expected, 15.7 mag on Dec. 18 (Ken-ichi Kadota). It keeps observable at 15-16 mag for a long time from 2005 spring to the end of 2006. Because it moves in the northern sky, it keeps observable for a long time in the Northern Hemisphere. It is brightest until May, but keeps lower than 30 deg high.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  22  3.67   53 58.4   3.583   3.208    60   15.6   4:53 (222, 28)  
Mar. 18  22 22.39   53 55.1   3.628   3.212    57   15.6   4:43 (222, 28)  

* C/2004 Q2 ( Machholz )

It was fantastic, so bright as 3.5 mag, so large as 30 arcmin, locating high overhead at its best time in early 2004 January. Then it has been getting fainter gradually, and become already too faint to see visually. However, it is still bright as 15.6 mag by CCD observations (Mar. 4, Katsumi Yoshimoto). It keeps observable until October when it becomes fainter than 18 mag.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  17  1.05    1  8.9   4.939   5.135    95   15.6   4:53 (336, 54)  
Mar. 18  17  1.06    1 27.1   4.899   5.200   102   15.6   4:43 (344, 55)  

* P/2004 VR8 ( LONEOS )

Although it was faint as 18 mag at the discovery in 2004 November, then it brightened very rapidly until early 2005, and reached to 16.0 mag on May 7 (Ken-ichi Kadota). After it appeared in the morning sky again, it continued brightening furthermore, and reached to 14.7 mag on Nov. 22 (Ken-ichi Kadota). It is also visible visually as 14.0 mag (Feb. 27, Seiichi Yoshida). After this, it keeps bright as 14-15 mag for a long time until spring. In the Northern Hemisphere, it keeps observable in good condition until summer when it becomes too faint.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  14  5.50   14 15.5   1.966   2.791   138   15.8   2:52 (  0, 69)  
Mar. 18  14  2.10   14 39.4   1.948   2.819   144   15.9   2:21 (  0, 70)  

* 174P/(60558) 2000 EC98 ( Echeclus )

It had been an extremely faint Centaur asteroid until 2004, fainter than 21 mag. However, it brightened up to 17.5 mag on 2005 Dec. 30, and a coma was observed, then it was revealed to be a comet. It brightened furthermore, 14.8 mag on Jan. 7 (Ken-ichi Kadota). It was also visible visually at 14.4 mag (Jan. 8, Seiichi Yoshida). It looked like a planetary nebula. It was diffuse visually. It seems to be a temporary brightening in outburst. It kept bright at 14 mag until early February, but it faded down to 15.4 mag on Feb. 28 (Giovanni Sostero and Ernesto Guido). It will return to be so faint as 21 mag in the near future. It will pass the perihelion in 2015. The heliocentric distance reduces down to 5.9 A.U., but it will be 17 mag at best. However, another outburst may happen again in the future.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  13 14.45   -5 50.4  12.071  12.947   150   15.8   2:01 (  0, 49)  
Mar. 18  13 13.05   -5 40.7  12.006  12.935   158   16.2   1:32 (  0, 49)  

* C/2004 D1 ( NEAT )

It brightened faster than a typical comet, and it reached to 15.8 mag on Feb. 9 (Ken-ichi Kadota). It will be observable in good condition as 16 mag for a long time until next spring.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  10 27.90   66 51.7   4.459   4.979   116   16.0  23:11 (180, 58)  
Mar. 18  10 23.54   66 29.0   4.510   4.982   112   16.0  22:39 (180, 59)  

* 73P-G/Schwassmann-Wachmann 3

Second sub-component recovered on Feb. 20. Although it was fainter than 19 mag on Feb. 9, it was already bright as 18.1 mag on Feb. 13 (Ken-ichi Kadota). It brightened rapidly up to 17.5 mag on Feb. 25. It can be the component E, one of the split components born in outburst in 1995. If it is the component E, it is fainter than its last appearance in 2001 by 3-4 mag. But it will reach to 8.5 mag at the encounter with the earth in May. However, the component E faded before the perihelion passage in 2001. So the future brightness evolution is very uncertain.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  14  4.22   15 18.4   0.640   1.534   138   16.9   2:51 (  0, 70)  
Mar. 18  14 12.25   16 50.7   0.552   1.468   141   16.2   2:31 (  0, 72)  

* P/2005 R2 ( Van Ness )

Although it was reported so faint as 17 mag at the discovery on Sept. 10 (M. E. Van Ness), it brightened rapidly and became so bright as 12.8 mag and visible visually in October (Oct. 24, Seiichi Yoshida). However, then it has been fading rapidly. It seems to have brightened temporarily in outburst. It faded down to 17-18 mag by CCD observations in January. Toni Scarmato reported it was 16.0 mag on Jan. 25, but extremely diffuse as DC=1. However, another small outburst occured again now. It somewhat brightened up to 15.6 mag on Feb. 12, and the central condensation became strong again (Ken-ichi Kadota).

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   2 45.70   24 58.0   3.698   3.262    56   16.3  19:27 ( 96, 39)  
Mar. 18   2 54.83   25 21.8   3.805   3.287    52   16.5  19:33 ( 99, 34)  

* C/2004 K1 ( Catalina )

It was visible visually as 14.3 mag in 2005 spring (July 10, Edwin van Dijk). Now it is 16.6 mag (Feb. 5, Ken-ichi Kadota). Although it keeps 16.5 mag from December to early April, then it will fade out rapidly, and become fainter than 18 mag in July.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  12 31.12   16 52.9   3.150   4.093   159   16.4   1:19 (  0, 72)  
Mar. 18  12 17.00   17 52.6   3.171   4.128   161   16.5   0:37 (  0, 73)  

* C/2005 K1 ( Skiff )

It had been observed at 16 mag by CCD, or 14 mag visually, in spring and summer in 2005. Now it is appearing again in the morning sky. It will be observable again at 16 mag in spring and summer in 2006. But the altitude will be somewhat lower than in 2005.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  19 31.00   -0 36.8   4.249   3.821    58   16.5   4:53 (295, 31)  
Mar. 18  19 35.31   -1  5.3   4.176   3.837    63   16.4   4:43 (298, 33)  

* C/2002 VQ94 ( LINEAR )

It passes the perihelion in 2006 February. But it is outside of Jupiter's orbit. So it keeps 17 mag for a long time. Because it moves in the northern sky, it keeps locating high and observable in good condition until 2006 summer.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  15 18.00   69  6.0   6.484   6.800   104   16.6   4:04 (180, 56)  
Mar. 18  15 10.25   69 27.7   6.491   6.801   104   16.7   3:29 (180, 56)  

* 32P/Comas Sola

It has already gone far away, and it must have been around 19 mag in calculation. Actually, it was so faint as 18.3 mag on Jan. 8 (Ken-ichi Kadota). However, an unexpected outburst happened and it brightened up to 15.7 mag on Jan. 27 (Ken-ichi Kadota). Then it has been fading rapidly, but it is still bright as 16.6 mag on Feb. 25. Probably it is observable brighter than 18 mag until April.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  15  6.55   -9 33.1   2.745   3.389   122   16.7   3:53 (  0, 45)  
Mar. 18  15  4.58   -9 26.8   2.699   3.428   130   16.9   3:24 (  0, 46)  

* (944) Hidalgo

It reached to 13 mag and was observed visually in good condition in 2004 autumn. It has been not observable since August, but it is appearing at dawn again. It keeps 17 mag until late April. But it will go away soon after that. Next return is in 2018, when it will be 14.3 mag at best.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  13 20.03    6 21.7   3.150   4.048   150   16.8   2:07 (  0, 61)  
Mar. 18  13 14.09    6 26.2   3.149   4.090   158   16.8   1:34 (  0, 61)  

* C/2005 N1 ( Juels-Holvorcem )

It reached to 11.4 mag in August (Aug. 12, Juan Jose Gonzalez). It was expected to start fading since early September. But actually, it keeps bright as 11.8 mag still on Oct. 7 (Juan Jose Gonzalez). Because it had been very low in the morning, it was not observed visually after that. Now it faded down to 16.6 mag (Jan. 28, Katsumi Yoshimoto). It will be close down to 0.4 degree to 129P, another 17 mag comet, and will be in the same CCD field on Mar. 16.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  12 42.81  -10 54.6   2.110   3.041   155   16.9   1:30 (  0, 44)  
Mar. 18  12 32.23  -11 10.5   2.151   3.118   163   17.1   0:52 (  0, 44)  

* 41P/Tuttle-Giacobini-Kresak

Great outburst over 6 mag has occured always in recent appearances in 1995 and 2001. The ephemeris says it will be 14 mag at best, but the actual brightness evolution will not be along the prediction. It is expected to be visible visually due to an unpredicted outburst again in this return. It is 16.6 mag on Mar. 3 (Toni Scarmato), already brighter than this ephemeris. Although it will not approach to the earth so much in this return, it keeps observable all through the period in the evening sky until autumn. It becomes brightest in June and too faint in autumn. It keeps locating around 30 degree high after May.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   5 31.97   19 14.9   1.176   1.580    93   17.4  19:27 ( 49, 68)  
Mar. 18   5 39.44   20 15.2   1.186   1.521    88   17.1  19:33 ( 62, 64)  

* C/2005 G1 ( LINEAR )

It was observed as 17.6 mag on Jan. 3 (Ken-ichi Kadota). It will be observable at 18 mag in good condition until May.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  14  6.34   70 25.7   4.556   4.962   108   17.4   2:54 (180, 55)  
Mar. 18  13 40.89   71 32.3   4.574   4.963   107   17.5   2:01 (180, 54)  

* C/2006 CK10 ( Catalina )

Although it is not observable around the perihelion passage, it is observable at 17-17.5 mag in good condition both in spring and autumn.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  12 17.98   62 29.4   1.599   2.271   120   17.6   1:08 (180, 63)  
Mar. 18  11 13.38   66  1.0   1.609   2.218   114   17.5  23:23 (180, 59)  

* 2006 BZ8

Peculiar asteroid with a comet-like orbit. Although it is not observable around the perihelion passage, it will reach to 17.5 mag only in a short time around March and November.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   9 47.40   26 50.7   1.368   2.269   147   17.5  22:28 (  0, 82)  
Mar. 18   9 12.04   29 36.4   1.428   2.229   132   17.8  21:26 (  0, 85)  

* 119P/Parker-Hartley

It reached to 17 mag in 2004 autumn. Although it has been not observable for a while, now it is observable as 17 mag in good condition again. It was reported as 18 mag recently, fainter than this ephemeris by about 1 mag.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11   7 11.16   17  5.9   2.826   3.391   116   17.7  19:55 (  0, 72)  
Mar. 18   7 12.98   17  8.9   2.931   3.405   110   17.8  19:33 (  3, 72)  

* 99P/Kowal 1

It is observable at 17.7 mag in 2006 spring. It is also observable at 17.5 mag in 2007 spring, but the altitude will be a bit lower.

Date(TT)  R.A. (2000) Decl.   Delta     r    Elong.  m1   Best Time(A, h)  
Mar. 11  11 23.23    7 44.8   3.867   4.859   176   17.7   0:11 (  0, 63)  
Mar. 18  11 19.77    8  3.0   3.870   4.853   169   17.7  23:35 (  0, 63)  

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