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(.#125).- Canditates for the Source of the 1977 WOW Signal Antonio Paris.
Canditates for the Source of the 1977 WOW Signal- Antonio Paris.
Antonio Paris
Washington Academy of Sciences
Hydrogen Clouds from Comets 266/P Christensen and P/2008 Y2
(Gibbs) are Candidates for the Source of the 1999 ‘’WOW’’ Signal
Antonio Paris
St. Petersburg College
Evan Davies
The Explorers Club, 46 East 70th St, New York, NY
Published Winter 2015
Abstract
On 1977 August 15, the Ohio State University Radio
Observatory detected a strong narrowband signal northwest of the globular star cluster M55 in the constellation Sagittarius (Sgr) [1]. The frequency of the signal, which closely matched the hydrogen line (1420.40575177 MHz), peaked at approximately 23:16:01 EDT [2]. Since then, several investigations into the “Wow” signal have ruled out the source as terrestrial in origin or other objects such as satellites, planets and asteroids. From 1977 July 27 to 1977 August 15, comets 266P/Christensen and P/2008 Y2 (Gibbs) were transiting in the neighborhood of the Chi Sagittarii star group. Ephemerides for both comets during this orbital period placed them at the vicinity of the “Wow” signal [3]. Surrounding every active comet, such as 266P/Christensen and P/2008 Y2 (Gibbs), is a large hydrogen cloud with a radius of several million kilometers around their nucleus [4]. These two comets were not detected until after 2006, therefore, the comets and/or their hydrogen clouds were not accounted for during the “Wow” signal emission. Because the frequency for the “Wow” signal fell close to the hydrogen line, and the hydrogen clouds of 266P/Christensen and P/2008 Y2 (Gibbs) were in the proximity of the right ascension and declination values of the “Wow” signal, the comet(s) and/or their hydrogen clouds are strong candidates for the source of the 1977 “Wow” signal.
Introduction
ON 1977 AUGUST 15 at approximately 23:16:01 EDT, the Big Ear Radio Telescope at The Ohio State University detected an intermittent narrowband radio signal (<1 0 KHz) northwest of the globular star cluster M55 in the constellation of Sagittarius (Sgr) and approximately 2.5° south of the Chi Sagittarii star group [5]. Determining the exact location where the 72- second signal originated from in the sky was problematic because the telescope used two separate feed horns to search for radio signals [5]. The data from the signal, moreover, was processed in such a way that it was difficult to establish which of the two horns detected the signal [2]. There are, therefore, two possible right ascension values for the source of the alleged extraterrestrial intelligence signal: 19h 22m24.64s ± 10s and 19h 25m17.01s ± 10s and the declination was determined to be −27°03′ ± 20 (Table 1) [2]. Two similar values for the signal’s frequency were assigned: 1420.356 MHz and 1420.4556 MHz. These two frequencies fall close to the hydrogen line, which is 1420.40575177 MHz [6].
Table 1: Right Ascension and Declination Equinox
Conversions; and Galactic Coordinates for the “Wow” Signal
(Source: Ohio State University Big Horn Report).
Declination Positive Horn Negative Horn
B1950.0 Equinox −27°03′± 20' 19h 22m24.64s ± 10s 19h 25m17.01s ± 10s
J2000.0 Equinox −26°57′± 20' 19h 25m31s ± 10s 19h 28m22s ± 10s
Galactic Latitude N/A -18d 53.4m ± 2.1m -19d 28.8m ± 2.1m
Galactic Longitude N/A 11d 39.0m ± 0.9m 11d 54.0m ± 0.9m
Previous Investigations by the Astronomical Community
Subsequent research to re-detect and identify the “Wow” signal by The Ohio State University, the Very Large Array, and The University of Tasmania’s Mount Pleasant Radio Observatory were null. After a search of the area where the “Wow” signal was detected (Table 2), the Very Large Array and The Ohio State University Radio Observatory concluded there was strong evidence against the origin of the source as terrestrial in nature or objects such as planets, man-made spacecraft, artificial satellites, and radio transmissions emanating from Earth. Furthermore, the Very Large Array proposed the intermittent “Wow” signal matched the signature of a transiting celestial source [5], while The University of Tasmania suggested the signal was moving with the source of the hydrogen line [7].
Table 2 : Right Ascension and Declination Observations Grid by the VLA and Ohio State (Source: VLA and Ohio State).
Date of Search RA DEC
VLA 25 SEP 1995 19h 21m28.1s to 19h 25m48s -27°41 to -26°18
07 MAY 1996 19h 21m28.1s to 19h 25m48s -27°41 to -26°18
Ohio State U. 05 OCT 1998 19h 22m22s -27°03
09 OCT 1998 19h 25m12s -27°03
9-10 APR 1999 19h 25m12s -26°48
17-18 MAR 1999 19h 22m22s -27°18
20-21 MAR 1999 19h 25m12s -27°18
22-23 MAR 1999 19h 22m22s -26°48
Anatomy of a Comet and Its Hydrogen Cloud
The distinctive parts of a comet include the nucleus, coma, dust tail, ion tail, and a hydrogen cloud. Moderately active comets are surrounded by a widespread cloud of neutral hydrogen atoms. The hydrogen is released from the comet when ultraviolet radiation from the Sun splits water vapor molecules released from the nucleus of the comet into the constituent components oxygen and hydrogen [8]. The size of the hydrogen cloud is determined by the size of the comet and can extend over 100 million km in width, such as the hydrogen cloud of comet Hale Bopp [9]. As a comet approaches the Sun, its hydrogen cloud increases significantly. Since the rate of hydrogen production from the comet’s nucleus and coma has been calculated at 5 x 1029 atoms of hydrogen every second, the hydrogen cloud is the largest part of the comet [9]. Moreover, due to two closely spaced energy levels in the ground state of the hydrogen atom, the neutral hydrogen cloud enveloping the comet will release photons and emit electromagnetic radiation at a frequency along the hydrogen line (1420.40575177 MHz) [10].
Comets 266P/Christensen and P/2008 Y2 (Gibbs)
From 1977 July 27 to 1977 August 15, Jupiter-family comets 266P/Christensen and P/2008 Y2 (Gibbs) were transiting in the vicinity of the Chi Sagittarii star group and significantly close to the source of the “Wow” signal (Figure 1) [11]. Of significance to this investigation, the purported source of the “Wow” signal wasfixed between the right ascension and declination values
(Table 3) of comets 266P/Christensen and P/2008 Y2 (Gibbs). On their orbital plane, moreover, 266P/Christensen was 3.8055 AU from Earth and moving at a radial velocity of +13.379 km/s; and P/2008 Y2 (Gibbs) was 4.406 AU from Earth and moving at a radial velocity of +19.641 km/s (Figure 2) [3].
Figure 1: Location of Comets 266P and P/2008 from 1977 July 27 to 1977 August 15.
(Source: The Minor Planet Center and NASA JPL Small Body Database) [11].
Note: The diagram can not be reproduced here. We apologize! It can be found on the original:
planetary-science.org/wp-content/uploads/2016/01/Paris_Davies-H-I-Line-Signal.pdf
Table 3 : Right Ascension and Declination Values for Comets P/2008 Y2
(Gibbs) and 266P/Christensen (Source: Minor Planet Center).
Date RA DEC
P/2008 Y2 (Gibbs) 27 JUL 1977 19h 28m12s ± 10s -27°31
01 AUG 1977 19h 25m17s ± 10s -27°33
05 AUG 1977 19h 22m23s ± 10s -27°35
15 AUG 1977 19h 16m37s ± 10s -27°36
266P/Christensen 07 AUG 1977 19h 29m47s ± 10s -25°53
15 AUG 1977 19h 25m17s ± 10s -25°58
Figure 2: On 1977 August 15, comet 266P/Christensen was 3.8055 AU from Earth and comet P/2008 Y2 (Gibbs) was 4.406 AU from Earth (Source: JPL Solar System Dynamics Database) [12]
Note: The diagram can not be reproduced here. We apologize! It can be found on the original:
planetary-science.org/wp-content/uploads/2016/01/Paris_Davies-H-I-Line-Signal.pdf
The data regarding comets 266P/Christensen and P/2008 Y2 (Gibbs), therefore, strongly suggest either comet, or both, could be the source of the hydrogen line signal detected by the Ohio State University on 1977 August 15. Chemicals in comets emit radio waves. The hydrogen radio waves from a comet, such as from 266P/Christensen and P/2008 Y2 (Gibbs), travel through space akin to light. Therefore, radio telescopes, including the Big Ear Radio Telescope at The Ohio State University, could have intercepted them. It is noteworthy to comment, moreover, during observations of the area by the Very Large Array and The Ohio State University Radio Observatory (from 1995 to 1999), comet 266P/Christensen and P/2008 Y2 (Gibbs) were not in the neighborhood of the right ascension and declination values of the “Wow” signal (Table 4) [5], thus the hydrogen cloud from these two comets would not have been detected. Additionally, because the period for comet 266P/Christensen is 6.63 years and P/2008 Y2 (Gibbs) is 6.8 years [3], their orbital period could account for why the “Wow” signal was intermittent and not detected during subsequent searches of the area.
Conclusions
There is noteworthy data to propose that the hydrogen signal detected by the Big Ear Radio Telescope at The Ohio State University, specifically 1420.356 MHz and 1420.4556 MHz, emanated from the neutral hydrogen clouds of comets 266P/Christensen and/or P/2008 Y2 (Gibbs). There are, conversely, many unknowns the astronomical community will need to address to confirm the hydrogen clouds from these comets were the source of the 1977 “Wow” signal. To date, no observations have acquired and measured the size, mass and spectral signature, most critically, of these two comets. Additionally, in 1977 the Big Ear Radio Telescope was operating in drift scan mode. Consequently, if a comet (or any celestial object) was the source of the “Wow” signal, it should have been detected in the trailing beam after detection in the leading beam [13]. Comet 266P/Christensen will transit the neighborhood of the “Wow” signal again on 2017 January 25 and can be located at 19h 25m15.00s and declination −24°50′ at a magnitude of +23 [3]. On 2018 January 07, comet P/2008 Y2 (Gibbs) will also transit the neighborhood of the “Wow” signal. Comet P/2008 Y2 (Gibbs) can be located at right ascension 19h 25m17.6s and declination −26°05′ at a magnitude of +26.9 [3]. During this period, the astronomical community will have an opportunity to direct radio telescopes toward this phenomenon, analyze the hydrogen spectra of these two comets, and test the authors’ hypothesis.
Table 4 : Location of Comets 266P/Christensen and P/2008 Y2 (Gibbs) During VLA and Ohio State Observations (Source: The Minor Planet Center).
Date RA DEC
P/2008 Y2 (Gibbs) 25 SEP 1995 (VLA) 11h 42m +00°22'
07 MAY 1996 (VLA) 16h 11m -32°01'
05 OCT 1998(Ohio) 20h 12m -22°45'
09 OCT 1998(Ohio) 20h 15m -22°41'
9-10 APR 1999(Ohio) 22h 02m -13°19'
17-18 MAR 1999(Ohio) 21h 48m -14°42'
20-21 MAR 1999(Ohio) 21h 50m -14°31'
22-23 MAR 1999(Ohio) 21h 51m -14°24'
266P/Christensen 25 SEP 1995 (VLA) 15h 12m -20°31'
07 MAY 1996 (VLA) 18h 03m -27°28'
05 OCT 1998(Ohio) 22h 01m -14°09'
09 OCT 1998(Ohio) 22h 00m -14°12'
9-10 APR 1999(Ohio) 00h 24m +02°35'
17-18 MAR 1999(Ohio) 23h 56m -00°42'
20-21 MAR 1999(Ohio) 23h 59m -00°17'
22-23 MAR 1999(Ohio) 00h 03m +00°0
References
1. Shostak, Seth (2002). “Interstellar Signal from the 70s Continues to Puzzle Researchers”. archive.seti.org/epo/news/features/interstellar-signal-from-the- 70s.php accessed on 01 Oct. 2015.
2. Ehman, Jerry R. (2010). “Wow! Signal 30th Anniversary Report.” North American Astrophysical Observatory www.bigear.org/Wow30th/wow30th.htm accessed on 14 Oct. 2015.
3. The International Astronomical Union Minor Planet Center, Database: MPEC 2009- A03 P/2008 Y2 (Gibbs); MPEC 2008-U27 266P/Christensen. www.minorplanetcenter.net/ accessed on 21 Nov. 2015.
4. Centre for Astrophysics and Supercomputing. Cometary Hydrogen Cloud, COSMOS, Swinburne Astronomy, astronomy.swin.edu.au/cosmos/C/Cometary+Hydrogen+Cloud accessed on 12 Oct. 2015.
5. Gray, Robert; Marvel, Kevin (2001). “A VLA Search for the Ohio State ‘Wow’”. ApJ, 546 (2001) pp. 1171-1177 www.bigear.org/Gray-Marvel.pdf accessed on 4 Nov. 2015.
6. Chaisson, Eric, and McMillan, Steve. (2005) Astronomy Today. 7th edition. Upper Saddle River, NJ. Pearson/Prentice Hall pp. 458-459.
7. Gray, Robert H.; Ellingsen, Simon (2002). “A Search for Periodic Emissions at the Wow Locale”. ApJ, 578 (2002) pp. 967-971.
8. Palen, Stacy. (2012) Understanding Out Universe, 2nd edition, New York, W.W. Norton pp 228-230.
9. Lang, Kenneth R (2010). Hydrogen Cloud of a Comet. NASA’s Cosmos. Tufts University Press ase.tufts.edu/cosmos/view_picture.asp?id=1291 accessed on 01 Sept. 2015.
10. Tenn, Joe. (2015) Hendrik C. Van De Hulst. The Bruce Medalists. Sonoma State University phys-astro.sonoma.edu/brucemedalists/vandeHulst accessed on 01 Sept. 2015.
11. Comet Base Observations Catalogue for P/2008 Y2 (Gibbs); 266P/Christensen. cometbase.net/en/observation/index accessed 13 Sept. 2015
12. Jet Propulsion Laboratory Small Bodies Database. Ephemerides and Orbital Solutions for P/2008 Y2 (Gibbs); 266P/Christensen ssd.jpl.nasa.gov/sbdb.cgi accessed on 13Sept. 2015. 13. Private Communication, (2015) Childers, Russ, Chief Observer at the OSU Radio Observatory, 1989-1997.
Bios
Antonio Paris
Antonio Paris is a Professor of Astronomy at St. Petersburg College, FL; the Director of Planetarium and Space Programs at the Museum of Science and Industry in Tampa, FL; and the Chief Scientist at the Center for Planetary Science – a science outreach program promoting astronomy, planetary science, and astrophysics to the next generation of space explorers. He is a member of the Washington Academy of Sciences, the American Astronomical Society, the St. Petersburg Astronomy Club, FL; and the author of two books, Aerial Phenomena and Space Science.
Evan Davies is a fellow of both the Royal Geographical Society, The Explorers Club, and his popular space science writing has appeared in Wiley publications as well as Archaeology and Spaceflight magazines. He is the author of Emigrating Beyond Earth: Human Adaptation and Sp ace Colonization and has held a lifelong interest in space exploration.
F I N .
Canditates for the Source of the 1977 WOW Signal- Antonio Paris.
Antonio Paris
Washington Academy of Sciences
Hydrogen Clouds from Comets 266/P Christensen and P/2008 Y2
(Gibbs) are Candidates for the Source of the 1999 ‘’WOW’’ Signal
Antonio Paris
St. Petersburg College
Evan Davies
The Explorers Club, 46 East 70th St, New York, NY
Published Winter 2015
Abstract
On 1977 August 15, the Ohio State University Radio
Observatory detected a strong narrowband signal northwest of the globular star cluster M55 in the constellation Sagittarius (Sgr) [1]. The frequency of the signal, which closely matched the hydrogen line (1420.40575177 MHz), peaked at approximately 23:16:01 EDT [2]. Since then, several investigations into the “Wow” signal have ruled out the source as terrestrial in origin or other objects such as satellites, planets and asteroids. From 1977 July 27 to 1977 August 15, comets 266P/Christensen and P/2008 Y2 (Gibbs) were transiting in the neighborhood of the Chi Sagittarii star group. Ephemerides for both comets during this orbital period placed them at the vicinity of the “Wow” signal [3]. Surrounding every active comet, such as 266P/Christensen and P/2008 Y2 (Gibbs), is a large hydrogen cloud with a radius of several million kilometers around their nucleus [4]. These two comets were not detected until after 2006, therefore, the comets and/or their hydrogen clouds were not accounted for during the “Wow” signal emission. Because the frequency for the “Wow” signal fell close to the hydrogen line, and the hydrogen clouds of 266P/Christensen and P/2008 Y2 (Gibbs) were in the proximity of the right ascension and declination values of the “Wow” signal, the comet(s) and/or their hydrogen clouds are strong candidates for the source of the 1977 “Wow” signal.
Introduction
ON 1977 AUGUST 15 at approximately 23:16:01 EDT, the Big Ear Radio Telescope at The Ohio State University detected an intermittent narrowband radio signal (<1 0 KHz) northwest of the globular star cluster M55 in the constellation of Sagittarius (Sgr) and approximately 2.5° south of the Chi Sagittarii star group [5]. Determining the exact location where the 72- second signal originated from in the sky was problematic because the telescope used two separate feed horns to search for radio signals [5]. The data from the signal, moreover, was processed in such a way that it was difficult to establish which of the two horns detected the signal [2]. There are, therefore, two possible right ascension values for the source of the alleged extraterrestrial intelligence signal: 19h 22m24.64s ± 10s and 19h 25m17.01s ± 10s and the declination was determined to be −27°03′ ± 20 (Table 1) [2]. Two similar values for the signal’s frequency were assigned: 1420.356 MHz and 1420.4556 MHz. These two frequencies fall close to the hydrogen line, which is 1420.40575177 MHz [6].
Table 1: Right Ascension and Declination Equinox
Conversions; and Galactic Coordinates for the “Wow” Signal
(Source: Ohio State University Big Horn Report).
Declination Positive Horn Negative Horn
B1950.0 Equinox −27°03′± 20' 19h 22m24.64s ± 10s 19h 25m17.01s ± 10s
J2000.0 Equinox −26°57′± 20' 19h 25m31s ± 10s 19h 28m22s ± 10s
Galactic Latitude N/A -18d 53.4m ± 2.1m -19d 28.8m ± 2.1m
Galactic Longitude N/A 11d 39.0m ± 0.9m 11d 54.0m ± 0.9m
Previous Investigations by the Astronomical Community
Subsequent research to re-detect and identify the “Wow” signal by The Ohio State University, the Very Large Array, and The University of Tasmania’s Mount Pleasant Radio Observatory were null. After a search of the area where the “Wow” signal was detected (Table 2), the Very Large Array and The Ohio State University Radio Observatory concluded there was strong evidence against the origin of the source as terrestrial in nature or objects such as planets, man-made spacecraft, artificial satellites, and radio transmissions emanating from Earth. Furthermore, the Very Large Array proposed the intermittent “Wow” signal matched the signature of a transiting celestial source [5], while The University of Tasmania suggested the signal was moving with the source of the hydrogen line [7].
Table 2 : Right Ascension and Declination Observations Grid by the VLA and Ohio State (Source: VLA and Ohio State).
Date of Search RA DEC
VLA 25 SEP 1995 19h 21m28.1s to 19h 25m48s -27°41 to -26°18
07 MAY 1996 19h 21m28.1s to 19h 25m48s -27°41 to -26°18
Ohio State U. 05 OCT 1998 19h 22m22s -27°03
09 OCT 1998 19h 25m12s -27°03
9-10 APR 1999 19h 25m12s -26°48
17-18 MAR 1999 19h 22m22s -27°18
20-21 MAR 1999 19h 25m12s -27°18
22-23 MAR 1999 19h 22m22s -26°48
Anatomy of a Comet and Its Hydrogen Cloud
The distinctive parts of a comet include the nucleus, coma, dust tail, ion tail, and a hydrogen cloud. Moderately active comets are surrounded by a widespread cloud of neutral hydrogen atoms. The hydrogen is released from the comet when ultraviolet radiation from the Sun splits water vapor molecules released from the nucleus of the comet into the constituent components oxygen and hydrogen [8]. The size of the hydrogen cloud is determined by the size of the comet and can extend over 100 million km in width, such as the hydrogen cloud of comet Hale Bopp [9]. As a comet approaches the Sun, its hydrogen cloud increases significantly. Since the rate of hydrogen production from the comet’s nucleus and coma has been calculated at 5 x 1029 atoms of hydrogen every second, the hydrogen cloud is the largest part of the comet [9]. Moreover, due to two closely spaced energy levels in the ground state of the hydrogen atom, the neutral hydrogen cloud enveloping the comet will release photons and emit electromagnetic radiation at a frequency along the hydrogen line (1420.40575177 MHz) [10].
Comets 266P/Christensen and P/2008 Y2 (Gibbs)
From 1977 July 27 to 1977 August 15, Jupiter-family comets 266P/Christensen and P/2008 Y2 (Gibbs) were transiting in the vicinity of the Chi Sagittarii star group and significantly close to the source of the “Wow” signal (Figure 1) [11]. Of significance to this investigation, the purported source of the “Wow” signal wasfixed between the right ascension and declination values
(Table 3) of comets 266P/Christensen and P/2008 Y2 (Gibbs). On their orbital plane, moreover, 266P/Christensen was 3.8055 AU from Earth and moving at a radial velocity of +13.379 km/s; and P/2008 Y2 (Gibbs) was 4.406 AU from Earth and moving at a radial velocity of +19.641 km/s (Figure 2) [3].
Figure 1: Location of Comets 266P and P/2008 from 1977 July 27 to 1977 August 15.
(Source: The Minor Planet Center and NASA JPL Small Body Database) [11].
Note: The diagram can not be reproduced here. We apologize! It can be found on the original:
planetary-science.org/wp-content/uploads/2016/01/Paris_Davies-H-I-Line-Signal.pdf
Table 3 : Right Ascension and Declination Values for Comets P/2008 Y2
(Gibbs) and 266P/Christensen (Source: Minor Planet Center).
Date RA DEC
P/2008 Y2 (Gibbs) 27 JUL 1977 19h 28m12s ± 10s -27°31
01 AUG 1977 19h 25m17s ± 10s -27°33
05 AUG 1977 19h 22m23s ± 10s -27°35
15 AUG 1977 19h 16m37s ± 10s -27°36
266P/Christensen 07 AUG 1977 19h 29m47s ± 10s -25°53
15 AUG 1977 19h 25m17s ± 10s -25°58
Figure 2: On 1977 August 15, comet 266P/Christensen was 3.8055 AU from Earth and comet P/2008 Y2 (Gibbs) was 4.406 AU from Earth (Source: JPL Solar System Dynamics Database) [12]
Note: The diagram can not be reproduced here. We apologize! It can be found on the original:
planetary-science.org/wp-content/uploads/2016/01/Paris_Davies-H-I-Line-Signal.pdf
The data regarding comets 266P/Christensen and P/2008 Y2 (Gibbs), therefore, strongly suggest either comet, or both, could be the source of the hydrogen line signal detected by the Ohio State University on 1977 August 15. Chemicals in comets emit radio waves. The hydrogen radio waves from a comet, such as from 266P/Christensen and P/2008 Y2 (Gibbs), travel through space akin to light. Therefore, radio telescopes, including the Big Ear Radio Telescope at The Ohio State University, could have intercepted them. It is noteworthy to comment, moreover, during observations of the area by the Very Large Array and The Ohio State University Radio Observatory (from 1995 to 1999), comet 266P/Christensen and P/2008 Y2 (Gibbs) were not in the neighborhood of the right ascension and declination values of the “Wow” signal (Table 4) [5], thus the hydrogen cloud from these two comets would not have been detected. Additionally, because the period for comet 266P/Christensen is 6.63 years and P/2008 Y2 (Gibbs) is 6.8 years [3], their orbital period could account for why the “Wow” signal was intermittent and not detected during subsequent searches of the area.
Conclusions
There is noteworthy data to propose that the hydrogen signal detected by the Big Ear Radio Telescope at The Ohio State University, specifically 1420.356 MHz and 1420.4556 MHz, emanated from the neutral hydrogen clouds of comets 266P/Christensen and/or P/2008 Y2 (Gibbs). There are, conversely, many unknowns the astronomical community will need to address to confirm the hydrogen clouds from these comets were the source of the 1977 “Wow” signal. To date, no observations have acquired and measured the size, mass and spectral signature, most critically, of these two comets. Additionally, in 1977 the Big Ear Radio Telescope was operating in drift scan mode. Consequently, if a comet (or any celestial object) was the source of the “Wow” signal, it should have been detected in the trailing beam after detection in the leading beam [13]. Comet 266P/Christensen will transit the neighborhood of the “Wow” signal again on 2017 January 25 and can be located at 19h 25m15.00s and declination −24°50′ at a magnitude of +23 [3]. On 2018 January 07, comet P/2008 Y2 (Gibbs) will also transit the neighborhood of the “Wow” signal. Comet P/2008 Y2 (Gibbs) can be located at right ascension 19h 25m17.6s and declination −26°05′ at a magnitude of +26.9 [3]. During this period, the astronomical community will have an opportunity to direct radio telescopes toward this phenomenon, analyze the hydrogen spectra of these two comets, and test the authors’ hypothesis.
Table 4 : Location of Comets 266P/Christensen and P/2008 Y2 (Gibbs) During VLA and Ohio State Observations (Source: The Minor Planet Center).
Date RA DEC
P/2008 Y2 (Gibbs) 25 SEP 1995 (VLA) 11h 42m +00°22'
07 MAY 1996 (VLA) 16h 11m -32°01'
05 OCT 1998(Ohio) 20h 12m -22°45'
09 OCT 1998(Ohio) 20h 15m -22°41'
9-10 APR 1999(Ohio) 22h 02m -13°19'
17-18 MAR 1999(Ohio) 21h 48m -14°42'
20-21 MAR 1999(Ohio) 21h 50m -14°31'
22-23 MAR 1999(Ohio) 21h 51m -14°24'
266P/Christensen 25 SEP 1995 (VLA) 15h 12m -20°31'
07 MAY 1996 (VLA) 18h 03m -27°28'
05 OCT 1998(Ohio) 22h 01m -14°09'
09 OCT 1998(Ohio) 22h 00m -14°12'
9-10 APR 1999(Ohio) 00h 24m +02°35'
17-18 MAR 1999(Ohio) 23h 56m -00°42'
20-21 MAR 1999(Ohio) 23h 59m -00°17'
22-23 MAR 1999(Ohio) 00h 03m +00°0
References
1. Shostak, Seth (2002). “Interstellar Signal from the 70s Continues to Puzzle Researchers”. archive.seti.org/epo/news/features/interstellar-signal-from-the- 70s.php accessed on 01 Oct. 2015.
2. Ehman, Jerry R. (2010). “Wow! Signal 30th Anniversary Report.” North American Astrophysical Observatory www.bigear.org/Wow30th/wow30th.htm accessed on 14 Oct. 2015.
3. The International Astronomical Union Minor Planet Center, Database: MPEC 2009- A03 P/2008 Y2 (Gibbs); MPEC 2008-U27 266P/Christensen. www.minorplanetcenter.net/ accessed on 21 Nov. 2015.
4. Centre for Astrophysics and Supercomputing. Cometary Hydrogen Cloud, COSMOS, Swinburne Astronomy, astronomy.swin.edu.au/cosmos/C/Cometary+Hydrogen+Cloud accessed on 12 Oct. 2015.
5. Gray, Robert; Marvel, Kevin (2001). “A VLA Search for the Ohio State ‘Wow’”. ApJ, 546 (2001) pp. 1171-1177 www.bigear.org/Gray-Marvel.pdf accessed on 4 Nov. 2015.
6. Chaisson, Eric, and McMillan, Steve. (2005) Astronomy Today. 7th edition. Upper Saddle River, NJ. Pearson/Prentice Hall pp. 458-459.
7. Gray, Robert H.; Ellingsen, Simon (2002). “A Search for Periodic Emissions at the Wow Locale”. ApJ, 578 (2002) pp. 967-971.
8. Palen, Stacy. (2012) Understanding Out Universe, 2nd edition, New York, W.W. Norton pp 228-230.
9. Lang, Kenneth R (2010). Hydrogen Cloud of a Comet. NASA’s Cosmos. Tufts University Press ase.tufts.edu/cosmos/view_picture.asp?id=1291 accessed on 01 Sept. 2015.
10. Tenn, Joe. (2015) Hendrik C. Van De Hulst. The Bruce Medalists. Sonoma State University phys-astro.sonoma.edu/brucemedalists/vandeHulst accessed on 01 Sept. 2015.
11. Comet Base Observations Catalogue for P/2008 Y2 (Gibbs); 266P/Christensen. cometbase.net/en/observation/index accessed 13 Sept. 2015
12. Jet Propulsion Laboratory Small Bodies Database. Ephemerides and Orbital Solutions for P/2008 Y2 (Gibbs); 266P/Christensen ssd.jpl.nasa.gov/sbdb.cgi accessed on 13Sept. 2015. 13. Private Communication, (2015) Childers, Russ, Chief Observer at the OSU Radio Observatory, 1989-1997.
Bios
Antonio Paris
Antonio Paris is a Professor of Astronomy at St. Petersburg College, FL; the Director of Planetarium and Space Programs at the Museum of Science and Industry in Tampa, FL; and the Chief Scientist at the Center for Planetary Science – a science outreach program promoting astronomy, planetary science, and astrophysics to the next generation of space explorers. He is a member of the Washington Academy of Sciences, the American Astronomical Society, the St. Petersburg Astronomy Club, FL; and the author of two books, Aerial Phenomena and Space Science.
Evan Davies is a fellow of both the Royal Geographical Society, The Explorers Club, and his popular space science writing has appeared in Wiley publications as well as Archaeology and Spaceflight magazines. He is the author of Emigrating Beyond Earth: Human Adaptation and Sp ace Colonization and has held a lifelong interest in space exploration.
F I N .
