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COMET ISON OBSERVING CAMPAIGN (=CIOC) SBAG Update Jan – Jul 2013

The Comet ISON Observing Campaign (CIOC) led by a diverse team maximizes telescope observations. Explore NASA accomplishments and upcoming events. Visit CIOC website for regular updates and resources. Exciting opportunities for professional and amateur astronomers!

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COMET ISON OBSERVING CAMPAIGN (=CIOC) SBAG Update Jan – Jul 2013

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  1. COMET ISON OBSERVING CAMPAIGN (=CIOC) SBAG Update Jan – Jul 2013 CIOC Team established Jan 2013 at SBAG-8. Team has a mix of experiences, skillsets, and research specialties. Abundant contributions from early- and mid-SBAG scientists. Reports monthly to Lindley Johnson, Kelly Fast, and Jim Green. Members chosen from SBAG: Lisse, Fernandez, Battams, Kelley, Knight, Vervack, Warner, Yanamandra-Fisher, DiSanti. Mantra: Facilitate, facilitate, facilitate. Bottom line is to maximize the science returned from Comet ISON by involving every telescope in the solar system in ISON observations. CIOC Contact Info: http://www.isoncampaign.org(Committee & news) https://dnnpro.outer.jhuapl.edu/isonworkshop (Workshop)

  2. CIOC Achievements/Products • NASA-NSF Opportunity Letter: e.g. SMA, GEMINI • NASA KECK Public Call - 12 partial nights scheduled (MOWG :) • NASA IRTF Public Call – 200 hours over 39 nights now scheduled • NSO Solar Telescope Observing: Sunspot/Dunn; KPNO/McMath-Pierce; Big Bear • Mars Fleet: MRO,MAVEN, Curiosity, Opportunity, Mars Express(?). Bonus: Observing practice for Comet C/2013 A1 (Siding Spring) VERY close Mars approach in Oct 2014 • Mercury Fleet: MESSENGER to Obtain Near-Planet Comparison to Comet 2P/Encke • Solar Fleet: Hinode, SDO, SOHO, STEREO, following up on Comet 2011 W3 (Lovejoy) • NASA Spacecraft (Astrophysics): SWIFT, Deep Impact, HST, Spitzer, Chandra • CIOC Website (information, news, links, no archiving) http://www.isoncampaign.org • NASA CIOC Facebook page, blogs; Amateur involvement; CARA & other “professional amateurs” • NASA HQ EPO: Ask an Astronomer; Media Point of Contact – e.g. NHK, Discovery Channel, BBC, etc. • CIOC WORKSHOP: Aug 1-2, 2013 at APL https://dnnpro.outer.jhuapl.edu/isonworkshop/Home.aspx

  3. Comet ISON Observing Campaign Website New CIOC Website Established: http://www.isoncampaign.org • Latest news/updates about the comet • Updated lightcurve • Workshop information • Resources for amateur/pro-am/professional astronomers • Blog posts from CIOC Team members Almost 3,000pageviews in the first week since launch!

  4. Why Care About C/ISON 2012 S1? Mercury Sol Mars Earth • First passage of comet through inner solar system since formation and ejection • -- Long arc from discovery and pre-discovery astrometry • -- More detailed dynamical studies than most “dynamically new” comets • On a Sungrazing Orbit • -- Discovered much earlier than any previous sungrazer • -- Perihelion Nov 28, 2013 at a distance of 2.7 solar radii • ISON will have close encounters with Mars, Mercury, Sol, and Earth in 2013. • This combination of fortuitous observing circumstances for a highly pristine dynamically new Oort Cloud comet has not occurred in the modern era of solar system exploration (that started 50 years ago with the Mariner 2 flyby of Venus). Earth

  5. C/ISON has likely spent the 4.5 Gyr since its formation far from the Sun and the planets in the deep freeze of the Oort Cloud. For C/ISON to come from the depths of the Cloud, with more than a year’s notice, at ~62o inclination to the ecliptic and have close encounters with 3 of the 4 inner system planets and the Sun is incredibly rare, practically unique.

  6. C/ISON will provide an amazing spectacle and fantastic observing opportunity for the best planetary seat in the solar system, Mars, when it comes within 0.07 AU of the planet on 01 Oct 2013.

  7. From J.Y. Li, APL Special Observations of Comets #2 Potential MRO Observing Dates #1 Closest Approach to Mars Oct 2 Earth Visual Black-Out Earth Visual Black-Out

  8. MRO Observation Campaigns • Campaign #1: sometime week of Aug 18-24 • Characterize activity as comet crosses through water line • HiRISE: two scans but try to keep to 1 orbit • MCS, CRISM considering what their observation requirements would be • CTX/MARCI would ride along on what observations work for them • Campaign #2: September 29 and October 2 • Structure of the coma • Sept 29 is best viewing geometry for imaging, Oct 2 is C/A • Plan both days as a single campaign • HiRISE: three separate scans • MCS, CRISM considering what their observation requirements would be • CTX/MARCI would ride along on what observations work for them

  9. Comet ISON will be extremely well placed for observations by solar observatories in space and on the ground as it passes through perihelion at q = 0.0125 AU on 28 Nov 2013. The comet will pass within the coronagraph of the SOHO LASCO C3 camera shown here, close enough to vaporize the refractory dust in its coma and tail.

  10. Heliophysics spacecraft plans for ISON observations SOHO • Will observe continuously in LASCO C3 and C2 coronagraphs from Nov 27-30. • Requests have been made to DSN for extended realtime coverage during critical times (e.g. entering C3 fovand transiting C2) so that observations can be adjusted to accommodate brightness, etc. STEREO Will observe ISON from October 10 through perihelion with heliospheric imagers, coronagraphs and EUV imagers on twin spacecraft in different locations on the far side of the Sun. SDO Currently plans to off-point to observe the perihelion passage of ISON

  11. Comet C/2012 S1 ISON: (Almost) Surely a Spectacular View Lovejoy in late 2012 Credit: Colin Legg Expected view of ISON on Dec 10 Credit: Dave Eagle, www.eagleseye.me.uk

  12. Detailed Comet ISON Scheduling at IRTF and Keck

  13. Draft SBAG CIOC Findings We find that a small group of comet experts working together with NASA HQ, NASA's telescope assets, NASA's EPO teams, and the scientific community to facilitate the maximal production of scientific results during a bright comet's apparition is highly useful. The creation of websites, workshops, and focused scientific meetings has helped to improve communication between interested observers and researchers and tailor future measurements for maximal return, while keeping the public well informed. A novel method of producing immediately public data sets from the Keck and IRTF has been well subscribed, while s/c projects (e.g. MRO, MESSENGER, SDO/SOHO/STEREO have been actively contacted to help design, implement, and analyze ISON observations during upcoming close passages of Mars, Mercury, Sol, and the Earth.

  14. ISON Science Results Slides

  15. Results from the 10 April 2013 HST DDT observations of ISON. (Left)Li et al. (2013) Coma + nucleus WFC3 F606W (R-band) image of the comet with a 1/p profile removed, showing a simple, strong sunward asymmetry and trailing tail structure and little variation during the three 45-min long visits performed over 19 hrs. Finding a slowly varying coma dominated by emission from the (hottest) subsolar point is not unreasonable for a simple unprocessed spherical comet nucleus. The HST WFC3 IFOV is 40” x 40” wide. (Right)F438W/F606W 2-color map of the comet’s nucleus, coma, and tail regions. Blue denotes regions of higher relative F438W emission, or bluer material, and red denotes redder regions with higher F606W. There is a mystery here – particle size changes caused by sublimation and fragmentation, decreasing the size of emitted dust, should create bluer dust farther from the nucleus. (Gas emission lines are not important in these filters, so we can focus on coma dust changes.) The best alternative explanation is that very icy dust is being emitted from the nucleus, and the ice is rapidly sublimating from this dust, leaving behind a redder remnant.

  16. CO/CO2 Coma HST 0.606 µm image taken on (4/10/2013) at rh = 4.4 AU vs. Spitzer 4.5 µm image taken on (6/13/2013) at rh = 3.35 AU, indicating the large spatial extent of the extended neutral gas coma + anti-solar dust tail. Scale Bar = 100,000 km. Dust Tail Nucleus

  17. C/2012 S1 (ISON): C.M. Lisseet al. report the detection of comet ISON using the Spitzer Space Telescope (SST) on 13.00 – 23.12 Jun UT at 3.6 um (left) and 4.5 um (center) when the comet was rh = 3.34 AU distant from the Sun, 3.29 AU from SST, and 4.25 AU from the Earth, well outside the water ice line. ISON's Spitzer coma morphology was relatively compact and simple, with a linear anti-solar dust tail > 3x105km in length (left) and a 1/rho profile gas coma extending > 2 x 106km from the nucleus (right). No variability in our L-or M-band photometry at the 0.03 mag level over 24 hrs was seen. First detection of neutral gas emission form ISON. Assuming a CO2 coma from a nuclear sourcewith outflow at ~0.35 km/sec (Biveret al. 3/2013), Q(CO2) = 1.9 x 1026mol/sec, and Rnuc > 0.09 km. Assuming the gas coma consists primarily of CO from a nuclear source with outflow at ~0.35 km/sec, we find Q(CO) = 2.1 x 1027mol/sec, and a minimum nucleus effective radius of 0.17 km. (Lengthscales, |Qgas|, rh activity fit CO2 well.) 4.5 um 3.6 um 4.5 - 3.6

  18. What We Currently Know About Comet ISON • Dynamically New Sungrazing Comet on 1st Passage through Inner SS since its formation 4.5 Gya. Exceptional inner planet “tour”. • Small nucleus, 0.1 km < Rnuc< 2 km (needs > 0.5 km to survive 0.014 AU perihelion) • Active out to 8.3 AU, slightly inside the CO2 Ice Line. • Linear Dust Tail (small, fine dust) + (CO/CO2) Gas Coma > 106km in Extent • Q(CO) ~ 2x1027mol/sec or Q(CO2) ~2 x 1026 mol/sec=> Rnuc> 0.1 km • Activity Level vs Time has Stayed ~ Constant Over Last 3 Months • No obvious Rotational Modulation or Outbursts to Date • No obvious Jet Concentrations – Maybe a Sub Solar Point Enhancement? • Qdust ~ 500 kg/sec (= 1.3 x 1010 kg total loss, Sep 2012 – Jul 2013; => Rnuc> 0.2 km for 0.35 g/cm3 density nucleus) • Could Very Well be C/Kohoutek II, the Sequel • Could Outburst and Fragment Inside Water, Dust Ice Lines @ rh = 2.5, 0.05 AU

  19. About The “K” Word Being on its first passage through the inner system may very well be the reason for ISON's precocious activity yet small size (< 2 km radius, Li et al. 2013 CBET 3496) and simple outgassing pattern - the comet is little evolved since its formation, and contains relatively more highly volatile ices than a JFC or LP (few thousand year period) comet, which are much more water rich per kg of nuclear material. Rapid depletion of these highly volatile ices in the surface layers of the comet at heliocentric distances of 5 to 10 AU may also be why we could be observing a "Kohoutek-like comet”. As much as we may not want to mention this mysterious under-performer in the night skies, C/1973 E1 (Kohoutek) was actually a bright comet (min [V]~0) during its inner passage through the solar system and the subject of an extensive observing campaign. A dynamically new comet discovered outside the orbit of Jupiter (Marsden 1974), Kohoutek evinced an initally steep production rate slope, a leveling off of production at 3 to 4 AU inbound (Delsemme 1975), and a close passage by the Sun (q = 0.14 AU). Using the first generations of CCD optical and IR bolometer detectors, rough estimates of Kohoutek’s nuclear size on the order of a few km were found (A’Hearn 1975); it was measured to be highly productive in CO or CO2 (Q(CO or CO2)/QH2O~1, Feldman et al. 1974) and in dust (Qdust,max ~ 104 kg/sec, Ney 1974, Zeilik & Wright 1975). The parallels are striking. With ISON, we thus have the opportunity to solve a 40 yr old mystery using the latest modern detectors, while at the same time we could be observing the most primitive of solar system objects.

  20. Comet ISON C/2012 S1 • Discovered September 21, 2012 by VitaliNevski and ArtyomNovichonok • Used 0.4-m telescope at International Scientific Optical Network (ISON) near Kislovodsk, Russia • Pre-discovery image from Mt Lemmon on Dec 28, 2011

  21. Why is C/ISON 2012 Important (II)? • Projected to get very bright • Everything on its surface will sublimate near perihelion • Allowing for many observations not commonly observable for comets • Favorable viewing geometry for observing • Pre-perihelion from Mars, close approach 0.07 AU C.A. =10/1/2013 • Pre-perihelion from Mercury, close approach 0.24 AU C.A.=11/18/2013 • Very Close Solar Passage, within 0.008 AU (1.7RSun) C.A.=11/28/2013 • Post-perihelion from Earth, close approach 0.42 AU, almost passing directly above north pole C.A. = 12/26/2013 • Long lead time to perihelion • Discovered at 6 AU, more than 1 year before perihelion • Very long time to organize major observing campaign • Observations planned from nearly all possible platforms in all wavelengths (see http://sungrazer. nrl.navy.mil/index.php?p=ison)

  22. ISON Wordle (1)

  23. ISON Wordle (2)

  24. Backup ISON Big Science Picture Slides

  25. In this plot showing a 2.5 – 4.9 um EPOXI spectrum of comet C/2009 P1 (Garradd), the narrow blue vertical bars represent the 8 BRRISON photometric imaging passbands. Imaging of the comet by Spitzer on 13 Jun 2013 using the 10% wide IRAC 3.6 and 4.5 µm filters will help BRISSON plan its observing strategy. Ground based IRTF/SPeX 0.8 – 5.2 µm spectroscopy of the comet in October 2013 will help BRISSON perform its continuum subtractions and color corrections, and provide an independent measure of the comet’s flux in regions of high atmospheric transmission outside the H2O and CO2 emission features.

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