Linking Amateur and Professional Mars Observing Communities.
Volume 4; Issue 2
February 14, 1999
Dear Marswatch participant,
Two items in this latest installment of the newsletter:
(1) Groundbased support for Mars Global Surveyor camera calibration sought
(2) Latest B.A.A. Mars observing update
Also, remember that the 1998-1999 Marswatch Web Site is on line! To get to
the site, point (and bookmark!) your browser to:
David Knighton of the Astronomical League is keeping the posted images and other information updated.
As many of you know, Mars Global Surveyor (MGS) has just entered into its final mapping orbit, and will begin systematic, global observations of the planet very soon. First, however, a series of calibration observations will be conducted between March 1st to March 8th, so that mission scientists and engineers will best be able to properly convert the raw images of Mars into scientifically-calibrated units (like Watts per unit area per unit wavelength). Mars Global Surveyor team members are very interested in comparing their measurements to those from well-calibrated, groundbased images of Mars obtained during the same time period in support of the MGS calibration.
Here's a chance for groundbased observers to directly support and enhance the results of an ongoing Mars spacecraft mission!
What can you do to help? What the MGS investigators need are accurate measurements of the magnitudes of different regions of the surface of Mars between March 1 and March 8, obtained through standard astronomical (UBVRI) filters. Especially important is the R filter, as this filter's bandpass is very close to that of the Mars Orbiter Camera's narrow angle camera bandpass.
To contribute to this effort, you will need a CCD camera and UBVRI filter set. You will also need to observe one or two well-characterized UBVRI standard stars near Mars, preferably either 16 Librae (BS 5570), or Beta Librae (BS 5685), and software for converting the star and Mars data into magnitudes. Color data for both these stars can be found at, for example, http://marswatch.tn.cornell.edu/ubvri.html
And, you will also need to obtain CCD calibration data (darks, flats) so that the Mars and star images can be properly reduced.
The MGS team does not have the resources or personnel to calibrate and reduce your images, so you would have to provide calibrated data, along with descriptions of the observations and observing circumstances, your equipment, and your data reduction procedures. Especially important also would be your estimates of the uncertainties in your magnitudes, arising from thin clouds, seeing variations, instrumental errors, tracking errors, etc.
This is a challenging set of observations to make, but it is well within the limits of many of today's advanced amateur astronomers, some of whom routinely obtain magnitude data for variable stars, asteroids, and other objects. Also, teachers and students out there: this would be an excellent project for an undergraduate astronomy course, and it could have tangible and practical benefits well beyond campus...
If you think you will be able to contribute and you would like more information on the MGS observations and the team's requirements, please send an email to Ed Danielson at email@example.com. For more information and guidance on obtaining calibrated magnitude data, please email Jim Bell at firstname.lastname@example.org. Time is short, however, as the MGS calibration period is only about two weeks away! Please pass this annoucement along to others whom you think might be interested in participation.
Latest B.A.A. Mars Observing Update: Mars Section Circular 1998-99, No. 3
By: Richard McKim, Director, B.A.A. Mars Section
Here is the most recent compilation of observations to date, from Richard McKim of the British Astronomical Association. This and earlier reports can also be found on the B.A.A. Mars reports page, at http://marswatch.tn.cornell.edu/baa.html
British Astronomical Association Mars Section Circular 1998-99, No. 3 December 16, 1998 - January 31, 1999
This Circular summarises the period 1998 December 16 - 1999 January 31 (Ls = 71 - 91 deg., D = 5.7- 7.8 arcsec., lat. of centre of disk 24 -18 deg. N). I have received CCD images from Don Parker, Frank Melillo and Damian Peach; David Gray remains the most prolific visual contributor. The weather in the UK has not been very cooperative, but observers have made the most of any fine weather. From Hawaii Nicolas Biver put his 26-cm reflector to good use on a few mornings. The OAA CMO 211 described Japanese work during December 16 to January 15.
The next Circular will discuss observations done in 1999 February, and I intend to compile it by March 7. Therefore please send any relevant work in time for it to be included. Most of the Circulars from the last apparition (and Nos. 1 and 2 from 1998-99) are to be found on the Mars Section website. There is a new MarsWatch site, now sponsored by the Astronomical League (http://www.astroleague.org/marswatch/). There is an article about how to observe the current apparition in the latest copy of the ALPO Journal (1998 October).
I hope to say something about the current round of Mars-bound spacecraft,
later, perhaps in the next Circular.
North Polar Region.
The cap remains bright and conspicuous, though the latitude of the S. edge has moved much further north. On January 11 for example, Warell found it to be "brilliant white". Parker's images (e.g., January 20, under CM = 66-69 deg.) also show the dark patch Hyperboreus Lacus at the edge of the cap. Though the tiny disk militates against really detailed study, Parker's CCD work indicated some detached outliers to the S. of the cap, and detail within the cap itself. Thus on December 25, CM = 310 deg., the cap had a well-defined brighter patch following the CM with indications of further structure around the centre of the cap. This bright spot seems to be a seasonal feature, and it was shown in Parker's red filtered images as well as in the overall composited colour views.
The most famous (and largest) seasonal outlier is Olympia. Antoniadi found it began to be separated from the cap near Ls = 80 and that the outlier could be followed up to Ls = 195. It is important to try to establish these seasonal dates for every favourable apparition, as some authorities have considered them variable from martian year to year. Further, being in fixed topographic positions, they provide another means of judging the seasonal progress of the polar cap. Parker's images of January 9 (CM about 170 deg.) imperfectly resolved Olympia at Ls = 81 degrees. Further observations please!
A new study of the NPC recession from Earth-based and HST data covering the
years 1990 to 1997 has recently appeared in Icarus (136, 175-191 (1998)).
Written by B.A.Cantor, M.J.Wolff, P.B.James and E.Higgs it advances evidence
that the recession rate varied slightly during these four apparitions, the
rate of recession being a bit slower in 1994-95. BAA NPC data from 1993 (and
1980-82) have already been published (R.J.McKim, J. Brit. Astron. Assoc.,
105, 117-134 (1995)), and recent (unpublished) analyses of the Section's
work for 1995 and 1997 suggests very small interannual differences during
1993-97. It is clear that the HST images are a quantum advance upon previous
Earth-based work, but being comparatively few in number it is still vital
that as many accurate measures as possible are made by ground-based workers.
Cantor et al. agree with the writer's opinion (expressed in the 1993 Section
Report, op. cit.) that measures of the north cap's E-W diameter involve
systematic errors (due to limb darkening or diurnal clouds) when the contour
of the cap is not located entirely within the visible disk. BAA data have
been analysed for the cap latitude on the CM (N-S direction): visual drawings,
filar micrometer data and measures from photographs, when made by the same
method have yielded comparable results. But comparisons of micrometric data
measured in the E-W sense have not agreed exactly. Thus historical comparisons
can present a problem if the method of measurement has not been stated in
the literature. In the course of his research for the BAA Dust Storm project,
among appropriately dusty archives in both the USA and Europe, the writer
found a great deal of unpublished polar cap data. Another project...?
No clear-cut evidence of dust storm activity has been found so far, but white cloud activity has increased, and there have been numerous records of the Equatorial Cloud Band (ECB) effect. The martian orographic clouds over Olympus Mons (Nix Olympica) and the Tharsis volcanoes have been very clearly imaged and observed visually. Rather than giving an incomplete preliminary meteorological report here, some selective notes of the more interesting observations are given below. All of Parker's work is CCD; the others, visual.
Parker, December 19: CM = 11-18 deg. Chryse-Xanthe is lightish, as is Tempe on the a.m. limb following M. Acidalium.
Parker, December 23: CM = 341-346 deg. Chryse-Xanthe is light on the morning side (especially in green and blue light).
Gaskell, December 24: Argyre is bright and bluish on the evening side, and there is extensive morning cloud over Tharsis to Solis Lacus.
Parker, December 25: CM = 310-318 deg. Hellas on the evening side looks only vaguely light. A thin ECB is seen across the disk.
Parker, January 1: CM = 250-256 deg. Elysium is light on the evening side. Hellas is only very slightly white in the morning, and there is some morning cloud over Aeria following Syrtis Major. In blue light (BG12) the Syrtis is invisible and the white cloud in Aeria enlarged. In an email Parker reports having seen the "Syrtis Blue Cloud" visually on this date.
Gray, January 7: CM = 122 deg. Nix Olympica, on the CM, is not especially light, but is seen to be surrounded by a dark area, especially on the N. side. (With a phase angle of 36 deg., the local martian time would be about 1.20 pm.) Tharsis, on the evening side, contains extensive bright cloud. The S. limb was rather light, too.
Parker, January 9: CM = 158 - 178 deg. Orographic clouds over the Tharsis region on the evening side, somewhat blurred by the seeing. Elysium is well onto the disk on the morning side and looks bright. (Allowing for phase it must be near local noon over Elysium.) These bright patches are imaged especially clearly in blue light.
Gray, January 10: CM =108-113 deg. Light S. limb. Tempe lightish on the p.m. side. Alba is light, crossing the CM. Nix Olympica on the a.m. side is also rather light
Warell, January 11: Argyre light on the evening side and extended haze over Memnonia on the morning side.
Parker, January 15: CM = 107-128 deg. The Equatorial Cloud Band effect is in evidence both in the blue light images and in the composited colour images. A bright equatorial cloud on the evening side thins out towards the west, and runs discontinuously across the disk where it meets a large bright cloud on the morning limb. The last images show a discrete Nix Olympica very bright approaching the CM (early afternoon, local martian time). Morning cloud also completely surrounds Propontis I, a phenomenon noticed in 1997, 95 and 93 (and illustrated in the 1993 final Section Report). Cebrenia is also hazy.
Gray, January 16: CM = 63 deg. The region just S. of Aurorae Sinus looks unusually pale as if affected by haze, but observing conditions are not perfect. On the evening side Chryse-Xanthe is a light region.
Parker, January 18: CM = 87-101 deg. ECB and Nix Olympica again very evident (blue, green light and in composited colour CCD frames). The evening cloud is over Xanthe and Candor-Ophir.
Parker, January 20: CM = 66-69 deg. Candor-Ophir is again light on the CM.
Gray, January 21: CM = 355 deg. The S. limb, including Noachis, is very bright, the brightness extending to encompass the small part of Argyre that is visible on the a.m. side. On the morning side this cloud extends north over part of M. Erythraeum. Chryse-Xanthe also bright on the morning side.
Gray, January 22: CM = 353-356 deg. Much as the 21st, but filter work shows
that the a.m. limb part of the S. limb brightness is most conspicuous in
blue and green light. (On both mornings this bright patch rapidly faded with
Propontis remains a conspicuous dark spot. Solis Lacus is still large and
dark to Parker, Gray and Biver, as it has been since the mid-80's. It is
elongated E-W. No internal details have been resolved yet. No trace has been
found of the Phasis development to the W. side of Solis Lacus, which is in
line with the gradual fade notice in the last few apparitions. As in 1997
the Cerberus region is not prominent, but it showed up faintly nonetheless
in Parker's CCD images, as well as in Gray's drawings. Gaskell reports having
picked up internal details in M. Acidalium.
Erratum in Circular No. 2
Apologies to David Gray for wrongly quoting the date of his Libya observation
as December 23: it should of course have read November 23.
Reporting data to the Section:
Send mail to Cherry Tree Cottage, 16 Upper Main Street, Upper Benefield, Peterborough PE8 5AN, Great Britain; home telephone 01832-205387; home email Rmckim5374@aol.com. Do not use the former email address for my place of work (which was email@example.com). You can also send any really urgent fax to my place of work on 01832-274052.
Richard McKim, Director, 1999 February 7
Jim Bell will continue to maintain the email distribution list as well as the various Cornell and JPL Marswatch-related WWW archives. If you are receiving duplicate copies of the International MarsWatch Electronic Newsletter, or you want your name added to or removed from the distribution list, please send him an email at firstname.lastname@example.org.
Department of Astronomy
Center for Radiophysics and Space Research
424 Space Sciences Building
Ithaca, NY 14853-6801
Phone: 607-255-5911; fax: 607-255-9002
Read the Next MarsWatch Newsletter (Volume 4; Issue 3; March 18, 1999)
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This page is maintained by David Knighton for the International MarsWatch. The 1998-1999 MarsWatch site it hosted by the Astronomical League as a service to the astronomical community. Comments, corrections, and suggestions can be addressed to email@example.com. This page last updated May 19, 1999.