New Criterion for Lunar Crescent Visibility

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1 New Criterion for Lunar Crescent Visibility Mohammad Sh. Odeh Islamic Crescents' Observation Project (ICOP) ABSTRACT A new criterion for lunar crescent visibility has been established using 737 observations, almost half of them obtained by the Islamic Crescent Observation Project (ICOP). This criterion is based on two variables, viz. the topocentric arc of vision and the topocentric crescent width. The new model is able to predict the visibility of the lunar crescent both for naked eye and optically aided observations. From the database we found a Danjon limit of 6.4 degrees. 1 INTRODUCTION The lunar crescent visibility has been studied by many astronomers since the Babylonian era, with as a result currently more than 12 different criteria for lunar crescent visibility, based on a number of sightings in different lunar conditions. Many of these criteria were developed by Islamic astronomers, since a number of Islamic religious events are directly related to lunar crescent sighting. For example, the new Lunar (Hijric) month begins on the next day of sighting the new crescent at west after sunset. 2 LUNAR CRECSENT VISIBILITY CRITERIA 2.1 Babylonian Criteria: The Babylonian deduced that the lunar crescent is visible by naked eyes if the two following conditions are satisfied at local sunset: 1- Age of the Moon is larger than 24 hours. 2- Lag time of the Moon (The interval time between sunset and moonset) is larger than 48 minutes. 2.2 Muslim Astronomers: Many Muslim astronomers had developed their own criteria or had studied and discussed the issue of the lunar crescent visibility in their literatures. Such as: Ibn Tariq, Habash, Al-Khwarzmi, Al-Khazin, Al-Tabari, Al-Fahhad, Al-Farghani, Thabet Bin Qurrah, Al-Battani, Ibn Maimon, Al-Biruni, Al-Sufi, Ibn Sina, At-Tusi and Al-Kashani (Ilyas 1994; Doggett & Schaefer 1994). For example, Ibn Tariq s criterion depends on the Moon s altitude at sunset and the Moon s lag time. In our modern time, Mohammad Ilyas developed several criteria for crescent visibility. 2.3 Recent and Modern Criteria: At the beginning of the 19 th century, Fotheringham and Maunder developed criteria for lunar crescent visibility, and in 1977 Bruin got his own criterion. Recently, Schaefer discussed the issue of the lunar crescent visibility extensively, and he included the atmospheric conditions in his work. Schaefer developed a criterion based on 295 observation records he obtained from several resources (Schaefer 1988, 1996; Doggett &

2 Schaefer 1994). Yallop (1997) used the same database which Schaefer established, but he made a comprehensive revision and corrections for some of the records. South African Astronomical Observatory (SAAO) developed a criterion based on Schaefer s database in addition to some other observation records from different resources (Caldwell & Laney 2001). 3 ISLAMIC CRESCENT OBSERVATION PROJECT (ICOP) The Islamic Crescent Observation Project (ICOP) was established in 1998 as a global project organized by the Arab Union for Astronomy and Space Sciences (AUASS) and the Jordanian Astronomical Society (JAS). Its primary aim as the only project of its kind is to gather information about the crescent observations at the start of each lunar month in different countries and regions through out the world. At the beginning of each lunar month, ICOP members send their results of observations to the coordinator of ICOP, and these results are being published immediately on the Internet at ICOP s home page at After seven years of extensive work for ICOP members, we were able to obtain a new large database for young lunar crescent observations. This database in addition to the old database were used to develop a new criterion to predict the visibility of the young lunar crescent, either by naked eyes or by optical aid. 4 VISIBILITY CRITERIA VARIABLES Below is a list of the most frequent observing parameters which have been used to predict the visibility of the lunar crescent. The three most basic parameters are shown in (Fig. 1):- Moon s age (Age): The interval time between conjunction and the time of observation. Moon s lag time (Lag): The interval time between sunset and moonset or moonrise and sunrise. Moon s altitude: The angular distance of the Moon above the horizon. Arc of light (ARCL): The angular separation (elongation) between the Sun and the Moon. Arc of vision (ARCV): The angular difference in altitude between the Sun and the Moon. Relative azimuth (DAZ): The angular difference in azimuth between the Sun and the Moon. Crescent width (W): The width of the lit area of the Moon measured along the Moon s diameter. The visibility of lunar crescent cannot be predicted reliably using only one of the above parameters. In particular, using Age or Lag only, as quite frequently done, has no predicting value at all, as shown clearly by (Schaefer 1996). At least two parameters should be used together in order to obtain accurate results, one related to the intrinsic brightness of the crescent, the other to its distance to horizon (itself closely related to atmospheric extinction).

3 Moon ARCV ARCL Horizon DAZ Sun Fig. 1: Basic geometric variables for crescent visibility prediction Contrary to a rather common assumption, the Moon's age is very poorly related to its intrinsic brightness. For example, a 10 hours Moon located on the ecliptic would have nearly the same brightness than a 0 hour Moon 5 degrees away from the ecliptic. A significantly better parameter for our purpose is the ARCL, since the width of the lunar crescent increases with the Moon's elongation from the Sun. It is not perfect however, since for the same ARCL, the width of the crescent is maximum when the Moon is at perigee and minimum at apogee. The best parameter for incorporating the Moon intrinsic brightness is thus directly the width (W) of the crescent. Regarding the second parameter, ARCV gives directly the angular distance of the Moon above the horizon and should be used in conjunction with W. Table 1, Table 2 and Table 3, show the criteria of Maunder, Indian and Bruin respectively. (Yallop 1997). DAZ ARCV Table 1: Maunder criterion DAZ ARCV Table 2: Indian criterion W 0' 3 0' 5 0' 7 1' 2' 3' ARCV Table 3: Bruin criterion Table 4 shows the SAAO criterion, where DALT is the apparent altitude, in degrees above the horizon, of the lower edge of the moon at sunset. If the crescent is below DALT2, naked-eye visibility will be improbable. Visibility with optical aid may be possible, but increasingly

4 unlikely approaching DALT1. Below DALT1, visibility is impossible even with optical aid. (Caldwell & Laney 2001). DAZ DALT DALT Table 4: SAAO Criterion 5 NEW LUNAR CRESCENT CRITERION I ve combined all the available lunar crescent observations into one large database, consisting of the following records:- 294 records from Schaefer list (Schaefer 1988, 1996; Doggett & Schaefer 1994). 6 records from Jim Stamm list (Private Communication). 42 records from SAAO list (Caldwell & Laney 2001). 15 records from Mohsen Mirsaeed list (Private Communication). 57 records from Alireza Mehrani list (Private Communication). 323 records from ICOP. So the new criterion is based on 737 records, and the visibility prediction is done adopting the following two variables: Airless Topocentric ARCV. Topocentric crescent width W. The 737 records are listed in Table 6, and the calculations were done using the software Accurate Times found at ( All the calculations were done at best time of observation, which can be approximated by the following equation (Yallop 1997): T b = T s + (4/9) Lag (5.1) Where: T b : Best Time T s : Sunset time Lag: Moon s lag time The new criterion is shown in Table 5. W 0.1' 0.2' 0.3' 0.4' 0.5' 0.6' 0.7' 0.8' 0.9' ARCV ARCV ARCV Table 5: New criteria Where:

5 Zone A (ARCV ARCV3): Crescent is visible by naked eyes. Zone B (ARCV ARCV2): Crescent is visible by optical aid, and it could be seen by naked eyes. Zone C (ARCV ARCV1): Crescent is visible by optical aid only. Zone D (ARCV < ARCV1): Crescent is not visible even by optical aid. Notice that ARCV1, ARCV2 and ARCV3 are airless and topocentric, thus the calculated ARCV must be the same as well. The visibility at the beginning of each zone highly depends on the atmospheric conditions, acuity of vision, experience of the observer and looking at the location of the crescent. That means you might not expect to see the crescent even by optical aid if your ARCV is just at the beginning of Zone C if the atmospheric conditions are hazy or unfavorable. Predicting the visibility of the lunar crescent by this new criterion can be also calculated using the following equation: V = ARCV - ( W W W ) (5.2) Where: ARCV: Airless and topocentric arc of vision in degrees. W: Topocentric crescent width in arc minutes. V 5.65 Zone A. 2 V < 5.65 Zone B V < 2 Zone C. V < Zone D. 6 LUNAR CRESCENT OBSERVATIONS DATABASE Table 6 below lists the 737 records, where Columns numbered 1 to 19 have the following meaning: 1 Record number, sorted chronologically. 2 Reference source, where: A (Schaefer list), B (Stamm list), C (SAAO list), D (Mirsaeed list), F (Mehrani list) and I (ICOP). 3 Morning (M) or evening (E) observation. 4 Local date of observation, in the form dd-mm-yyyy. 5 Name of the observer. 6 East longitude of the location of observation. 7 Latitude of the location of observation. 8 Elevation of the location of observation in meters. 9 Visibility by naked eye; Invisible (I), visible (V) or blank if not tried. 10 Visibility by binocular; Invisible (I), visible (V) or blank if not tried. 11 Visibility by telescope; Invisible (I), visible (V) or blank if not tried. 12 Julian date at the time of calculations (Best Time). 13 Topocentric age of the Moon (Age) in hours at Best Time.

6 14 Lag time of the Moon (Lag) in minutes Topocentric arc of vision (ARCV), topocentric relative azimuth (DAZ) and topocentric arc of light (ARCL), all in degrees at Best Time and are not corrected for refraction. 18 Topocentric crescent width (W) in arc seconds at Best Time. 19 Visibility prediction value (V) described in section 5.

7 Table 6: Lunar crescent observation records (Group D) No. R E Date Observer Long Lat Ele N B T JD Age Lag ARCV DAZ ARCL W V 514 I E Sehbajraktarevic I I E Odeh I I I E Sani I I E Fahmy I I E Katbeh I A E McPartian I F M Mehrani I E Khan I I E Chalermthai I I I E Al-Muhammad I I I I E Salie I I M Stamm I I E Hadi I I I E JAS I I I I E Dukku I A E Schaefer I I I E Hafiz I A E Stamm I I I E Lukuman I I E Pazhouhesh I I I I E Khushaish I I A M Schaefer I I I E Al-Muhammad I I I E Ebrahim I I I I E Kacem I I I E Janghorban I A M Stamm I I A E MacKenzie I A E Schmidt I I E Stamm I I I I E Saab I A E Stamm I I I E Stamm I I I E Salie I I E Al-Muhammad I I E Mayoof I I I I E Odeh I I I I E Dukku I I E Caldwell I I E Khan I I I E Ebrahim I I I E Ebrahim I A E Schmidt I A E Krisciunas I I F M Mehrani I I E Salih I

8 Table 6: Lunar crescent observation records (Group C) No. R E Date Observer Long Lat Ele N B T JD Age Lag ARCV DAZ ARCL W V 737 I E Stamm V I E Siddiqui I I E Kacem I I A E Schmidt I I E Kacem I I I E Al-Muhammad I I F E Mehrani I E Odeh I I I C E I I E Odeh I I I E Mehrani I A M Stamm I I I E Lukuman I I E Stamm I I F E Mehrani C E I I E Ebrahim I I M Stamm V I E Tirhi I I A E Schaefer I I I E Ebrahim I I I E Murad I I I E Marzani I I I E Salie I A E Stamm I I I E Caldwell I I I I E Farooq I I A E McPartlan I I E Ebrahim I I I E Amirzadeh I I E Singer I I I E Touma I A E Schmidt I I E Farooq I I I E Essa I I E Rahkooi I I I E Sarker I C E I A E McPartlan I I E Al-Muhammad I I I E Caldwell I I I E Muttardy I I E Salie V I E Ebrahim I I I E Alsup I I E Al-Muhammad I I I

9 647 I E Khushaish I I I E Khakoo I I E Essa I A E Schmidt I I E Odeh I B E Movahhed-Nezhad V I E Caldwell I I E Hadi I V D E Mirsaeed V A E Stamm I I F E Mehrani I I E Al-Muhammad I I I A M Krisciunas I I I E Hafiz I I E Katbeh I I F E Mehrani I I I E Stamm I V I E Stamm I I V I E Fathy I I E Khadraoui I F E Mehrani V A E McPartian I I E Kacem I I I C E I D E Mirsaeed I I E Odeh I I I E Touma I I D E Mirsaeed V I E Katbeh I I V D M Mirsaeed V D E Mirsaeed V I E Salie V I E Mehrani I V A E Stamm I V I E Odeh I I I I E Mohammadi I V C E I A E Pierce V V A E Bach I V A E Golden I I F E Mehrani I E Mehrani I V I E Mehrani I V A E Schwaar I V I E Mohammadi I I E Sani I A E MacKenzie I I E Dukku I F E Mehrani I

10 478 I E Odeh I V V A M Schaefer I I E Odeh I I V C E I I E Gharaybeh I F E Mehrani I V I E Hadidi I V I E Mohammadi I A E Patchick I V A E Patchick I I I E Al-Muhammad I I F M Mehrani I C E V A E Schmidt I I E Kacem I V A E McPartlan I A E Bach I V A E Schmidt I I E Odeh I V V F M Mehrani A E Schwaar I V F M Mehrani V Table 6: Lunar crescent observation records (Group B) 433 I E Salie V A E Pearce I V I E Salie V A E I A E Stamm I I A E Austin I V A E MacKenzie I C E I F M Mehrani I I E Isiaq I C E V I E Katbeh I I V I E Caldwell V I E Torabinejad I V I E Amirzadeh V A E Victor I V A E Heaslip I I A E Stamm I I A E I A E Hunefeld I V I E Odeh I V V A E Stamm I V I E Ebrahim I I I E Hafiz I

11 658 F M Mehrani I V I E Torabinejad I V A E McMahon I I A E Moran I V F M Mehrani I C E V I E Isiaq V B M Pearce V A E Schmidt I I E Boroujerdi I I E Essa I I E Bahali I V V I E Essa I D M Mirsaeed V I E Marzani I I A M Skiff I V I E Mohammadi I I A E Victor I V C E V D E Mirsaeed V F E Mehrani I F E Mehrani V I E Al-Muhammad I I C M I I E Haji Ali Ahmad I I I I E Mehrani I V C E V I E Khushaish I I A E Bieda I V A M Bortle I V I E Guessoum I B E Stamm V V I E Saab I I D M Mirsaeed V B M Stamm V A E Schmidt I I E Bahali I V V C E V A E Pearson I V A E Stamm I V I E Stamm V V V A E Schmidt I I E Kacem V V A E Schmidt I A E Stamm I V I E Mokhtari I B E Stamm V V I E Tahir I I V I E Stamm I V

12 436 I E Essa I I E Hadi I I V C E V C M V A E Bortle I V A E O'Meara V V C E V I E Mehrani I V A E Schmidt I C E V F M Mehrani A E Long V F E Mehrani I A E I A E Bishop V I E Haji Ali Ahmad I V A M Danjon I V A E Chamberlain I V F E Mehrani F M Mehrani V V I E Mohammadi I V I E Lukuman I I E Khushaish I I A E Stamm I V B E Pearce V A E ACAC V A E Olsen I V I E Ibrahim I V A E McPartian I I E Zainal I V I E Bahali I I V A E Sherman I V A E I I E Shaukat I V C E V A E Verne V I E Mohammadi I I E Kaufmann V V C E V A E Fcfferman I V C E V I E Al-Muhammad I I I E Odeh I I V I E Mayoof I V I E Kaufmann I V I E Stamm V V V F E Mehrani I E Odeh I V I E Mohammadi I V

13 218 C E Laing V I E Al-Muhammad I I A E V I E Pazhouhesh I V A E Bortle V V A E Dessert V A E Dombrowski V V A E Piaruli V C E V A E Klemola V A M Patterson V V D M Mirsaeed V I E Mehrani I V I E Isiaq I I E Salie V I E Caldwell V V D M Mirsaeed V A M Degroupet V A E Schenk V V A E Schmidt I I E Zainal I V V D E Mirsaeed V C E O'Meara V I E Salih V V I E Al-Mustafa V I E Mehrani V V I E Kacem I V I E Kacem I V I E Janghorban V A E Campbell V A E Schaefer V A E Schmidt I D M Mirsaeed V I E Caldwell V V I E Caldwell V V I E Salie V A E Schoch V A E Peterson V V I E Gharaybeh I I E Ebrahim V D M Mirsaeed V I E Nahli V I E Mehrani I V F M Mehrani C E V C E V I M Mehrani V I E Odeh V V I E Saab I V

14 574 I E Ebrahim V A E Triou V I E Saab I V V F M Mehrani V V A E Schmidt V I E Mohammadi V V I E Mehrani V V C M O'Meara V I E Janghorban V V V I E Mehrani V V V A E Cebula V A E Phelps V I M Khushaish V I E Caldwell V V I E Kaufmann V V I E Kacem V V I E Odeh I I V I E Kaufmann V V A E DeCroupet V A E McGraw V A E Newman V I E Shammary V V I E Mehrani V V I E Khushaish I V I E Salie V I E Odeh I V A E Oravec V V C M V A E Schaefer V V A E McLeod V V A E Doggett I A E Seidelman I I A E Slowik I A E Chester V V A E Schmidt V V A M Danjon V A E MacKenzie I A E Schmidt I A E Cave V C M Laing V I E Tahir I V V I E Bilani V V I E Saab I V A E Williams I I E Hasanzadeh V I E Ebrahim V D M Mirsaeed V I E Stamm V I E Salie V

15 108 A E MacKenzie V A E Denning V A E Westfall V V I E Kacem V V A E Caton I A E ASU V V A E ASU V A E Victor I V A E V V I E Ebrahim V I E Odeh V V I E Mehrani V V I E Kacem I V V I E Aram I V C E V A E Bac V A E Seidelman I I E Saab I V V A E Korycansky I V A E Haasdyk V I E Gharaybeh I I E Torabinejad V V A E Byrd I A E MacKenzie I A E Pitluga I I E Mohammadi V V C E V I E Mohammadi I A M Stamm I V C M V I E Dalee V V A E Richardson V I E Torabinejad V A E Johnson V A E Schmidt I Table 6: Lunar crescent observation records (Group A) 128 A E Quigley V V I E McKenna V V V I E Odeh V V A E Victor V I E Farooq V V A E Schmidt I I E Mehrani I V A E Fry I A E Barrett V A E Hill V V A E Talbert V

16 149 A E Connor V V A E Bohn V V I E Essa I I E Mwinyifaki V A E Sykes V C M V A E Watts V V A E Fleming V V D M Mirsaeed V A E McPartlan I A E Duncombe V A E Lampland V A E Guzman V A E Morris V I E Yucel V V I E Johnson V A E McGraw V A E Denning V A E Faber V V A E Olsen V V A E Bricker V V I E Kacem I V I E Zainal V V V A E Arnold V A E Keszthelyi V A E Stamm I V F M Mehrani V V A E Hoffler V A E V V A E Fleming V I E Qureshi V V I E Singer V V C E V C E V A E V V A E V A E McPartian I C E V A E Schmidt I I E Kaufmann V V A E Schmidt V C E V I E Singer V V I E Odeh V V A E Rosamond V V A E Schiffer V V A E Meibaum V A E Tshernov V A E Chamberlain V

EXPLANATION A10. The example (ii) Moonset shows that no moonset occurs in this position on January 23.

EXPLANATION A10. The example (ii) Moonset shows that no moonset occurs in this position on January 23. A10 EXPLAATIO In correcting for longitude to give the UT, it is sufficiently accurate to add or subtract 24 h, changing the Greenwich date by one day, to find the following or preceding phenomenon. Examples.