Planisphere and Star-Map with multi-projection, "hayami.exe" This is a Planisphere with 14 projection. You can use as star map, also as usual map. ============================== **REMARK** The format of .plt is changed since version-6. If you use old files, the program stops with error. Please change .plt-files in "Sun,Moom and Tech" -> "Planets", from all "prm***.plt" to "prm***2.plt". ============================== Index [A]Contents in Archives (Operations on the Main Window) [B]How to use in the left half easily. [C]How to use in the right half. [D]How to use in the left half in full. [E]Star Map mode and Earth Map mode (by each menu) [F]Projection [G]Sun,Moon and Tech [H]Display [I]File [J]Error on Operation [K]Technical matters [L]Reference [M]History ----------------------------- Index(in detail) [A]Contents in Archives (Operations on the Main Window) [B]How to use in the left half easily. 1)the Size of the Main Image 2)Magnification (Only for the case of 1) 3)Mode (Only for Nomal mode) 4)Longitude, Latitude and TIME ZONE of the ovservational place 5)Date and Time 6)"DRAW" 7)Clicking on the main image 8)End [C]How to use in the right half. 9)Comment 10)Asigning The center of Projection 11)Coloring or Centralizing by a Constellation 12)Keyword-Search in Star-Catalogue and Centralizing by it [D]How to use in the left half in full. 1)The Shape of the main image[Normal / Half-Height / Dual-box] 2)The sense of Magnification and How to assigning Magnigication 4)on TIME ZONE 6)"OverDRAW" 7)The window for Clicked point 7a)Displaying Coordinates 7b)Centralizing 7c)Search stars around the clicked point 7d)Radius of Click-Search 7e)Changing comments in Click-Search 7f)Click-Search in "DRAW using FILE" 7g)Mesurement by Click 7h)writing comments at the clicked point [E]Star Map mode and Earth Map mode 3b)Star-Map mode 3c)Earth-Map mode (by each menu) [F]Projection 13)Selecting Projection 13a-n)Explanation of each projection 13o)Azimuthal projection defined by user 13p)Remark 14)Upper or Lower Shift of the image 15)Displaying under the horizon 16)Direction of Vertical [G]Sun,Moon and Tech 17)Sun and Moon on the image 18)the Antipode of Sun and the shadow of Earth 19)Planets on the image 20)Star assigned by Coordinates 21)Object assigned by Orbital Elements 22)Displaying Coodinates of Sun, Moon, Planets in the Comment Area 23)Displaying Precession and Nutation in the Comment Area 24)Units in the Comment Area Remark)Size of the Comment Area [H]Display 25)Colors of Stars and Background 26)Lightness for displaying stars 26a)Size of Stars on the image 27)Lines of Constellations 28)Coordinate lines 29)Moon-Line 30)Longitude- and Latitude-line of Earth 31)Scale of Rectangular Coordinate 32)Refraction corretion 33)Diurnal Aberration correction 34)How to calculating the center of Constellation 35)"DRAW using FILE" 36)Setting for the click-window and minute options [I]File 37)Save and Load the Obsevational location 38)Save as bitmap image 39)Setting Star-Catalogue Files 40)End [J]Error on Operation [K]Technical matters [L]Reference [M]History ============================= [A]Contents in Archives READMEmj.txt:Explanation on hayami.exe(in Japanese) READMEme.txt:Explanation on hayami.exe(in English) READMEsd.txt:Explanation on strdrt.exe READMplt.txt:Explanation on .plt-file **Necessary File hayami.exe :the main program **Nesessary Files,but you can rewrite or change ET-UTC.txt :the data file on delta-T=(Dynamic Time)-(UT1 or UTC) ALLSTAR5.txt:Star Catalogue(lighter than mag 5.5, with constellation and star name) ALLSTAR7.txt:Star Catalogue(mag 5.5-7.5, the default file of the second Catalogue) ALLSTAR9.txt:Star Catalogue(mag 5.5-9.5, the replacement as the second Catalogue) zentend.txt :the dummy file same format as Star Catalogue but no data. seiza.txt :the list of constellations(Japanese) seiza-e.txt :the list of constellations(English) seiza-l.txt :the list of constellations(Latin) seiza-d.txt :the list of constellations(German without umulauts) seiza-du.txt:the list of constellations(German with umulauts) seiza-n.txt :the list of constellations(Dutch) seiza-f.txt :the list of constellations(French) seiza-i.txt :the list of constellations(Italian) senzanet.net:line data of constellation(in Coordinate) seizacpx.net:line data of constellation(in Coordinate, complex) prmprc.txt :the parameter file for Precession nutation.txt:the parameter file for Nutation prmmean2.plt:the parameter file for Mean Elements of Planets(in J2000.0) prmsun2.plt :the parameter file for location of Sun(in J2000.0) prmmon2.plt :the parameter file for location of Moon(in J2000.0) prm***2.plt :the parameter file for location of Planets(in J2000.0) (Mercury:prmmrc2.plt,Venus:prmvns2.plt, Mars:prmmrs2.plt, Jupiter:prmjpt2.plt,Uranus:prmurn2.plt,Neptune:prmnpt2.plt) **Other Files cnstlnet.exe:the program to translate from a file written in Catalogue-Star-numbers into a file written in Coordinates seizanet.txt:line data of constellation in Coordinates seizacpx.txt:line data of constellation in Coordinates(complex) ngc2000.frm :the format file for using NGC2000.0 directly on_ngc.txt :remark on ngc2000.frm circle.txt :data file for drawing many small circles to show skewness by a projection circle.frm :the format file for circle.txt oncircle.txt:remark on circle.txt and circle.frm cle.frm **Files, you may delete soon (city name).ini:location data file(long.,lat.,TIME ZONE,etc.) ******.str:Star data file I prepare Large Megellanic Cloud and Small Magellanic Cloud. ******.crd:Coordinate system data file I prepare Ecliptic and Galactic coordinates system. ******.orb:Orbit data file I prepare followings as Sample: geostatio.orb(synchronous orbit. Mean Anomaly equals to East longitude of the satellite) tuttle.orb(commet 8P/Tuttle,elliptical orbit), boethin.orb(comet 85P/Boethin,elliptical orbit), sidingsp.orb(Comet/2007 K3,Siding Spring,hyperbolic orbit) tokyo10828.txt:sample data for DRAW using File (the Moon in Aug.28th 2007, by Zenithal Coordinate) form_1.frm:format file for tokyo10828.txt ================================= [B]How to use in a left half easily. You boot the main program, then the crowded window appears. When you use it as Planisphere, you need the upper most quarter and the left half. (1)Enter "Size of Image" in pixels. The Area of Main Image is square of this size, but increase with Comment area, so total image become larger. (the left side, the upper side and the lower side grow 20pixels, the right side grow 260pixels, and plus MS-window area.) The initial size is 320pixels, then the actual size is 622pix*408pix. (2)You can enter "Magnification". But when you use it as usual Planisphere, "Magnification"=1. If more than 1, you must decide the center of the Magnification. I explain the detail in section [D]. (3)You can select one of 3 modes of "What you draw". 5-a) The Sky in the asigned time and location (as usual Planisphere) 5-b) Star map 5-c) Earth map I explain the detail of 5-b) and 5-c) in section [E]. (4)Enter the Longitude, the Latitude (in degrees), Altitude (in meters) and TIME ZONE (in hour and minute) of your observational location, and TIME ZONE of your PC. In usual usage, it is enough the accuracy of longitude and latitude are around 1degree, and you may set the altitude=0 meter. If you watch from a high mountain and you can see the sea horizon, set the actual altitude. You can know PC's TIME ZONE from "Time and Date" of MS-Windows, that apear when you click the clock of task bar. You can know also TIME ZONE of the observational location (if defferent from PC's TIME ZONE). Enter both. (5)You set the time that you want to know the sky. How to enter the time is followings: i)Enter year,month,day,hour,minute (for month, select in pull down). ii)Push "the Now" then the program reads the present time from PC. (if PC's TIME ZONE and actual TIME ZONE are different, the program calculates the time in the observational location.) iii)Push "before" or "after", then the time is adjasted with the number in the box before the bottons. In the box, the unit is m:minute, h:hour, d:day, w:week, y:year. The default unit is "m". (6)Push "DRAW", the image window appears. In the Initial setting the window is small, but you can spread to the size that you set. Scroll-bars is in different position from usual Window program. Sorry. (7)Click on the image, then another window appears and displays the Azimuth, the Elavation, RA, Dec, the Aberration, the Refraction and the nearest Constellation of the clicked point. (the Constellation is "the Constellation containing the nearest star from the clicked point in stars more lighter than Mag=5.5, so may be different from the area of Constellations.) If there are displayed stars in 1degree from the click point, the window displays the stars in ascending oder of distance (but up to 9 stars), with RA, Dec, the distance from the clicked point, and Magnitude. If the light star, the Constellation and the name may be displayed. When you display dark stars, the window become bigger, and you may wait a few seconds. If you change the setting but do not push "DRAW", and click the image, the window displays as same as the setting when drawing. When you use "OverDraw", the setting at the last drawing is used. (8)You push "x" at the upper right corner of the main window, then all windows close and finish. Then The followings are recorded in "hayami.ini": the size, data of the location, TIME ZONE, the time, Comment, Locations of 3 windows, and the size of the Image window. when the next boot, these are resumed. ======================================== [C]How to use in a right half. (9)If you write in "Comment", the comment is displayed in the right comment area. The comment is also recorded when closed or "Save Location". Use the comment on Location data. You can enter 60 letters. If more than 32 letters, the program cuts the comment to 2 lines, but may fail to display in the Image area. (10)In any Projection, the image is skew at the around, more than at the center. Thus you can change the center of the projection to the direction you want. In "The center of Projection", you enter the Azimuth (North=0deg,West=90deg,South=180deg,East=270deg) and the Elavation(Zenith=90geg,Horizon=0deg). Then the center of the Image is this derection (marked by blue "x"). You can enter a direction in RA and Dec, or Ecliptic Coordinate. Change the above pull down to the coordinate you want. If the direction become under the horizon, the alert apears, but the image is drawn according to the setting. Then the image may be all black. in default, the upper direction is the zenith (when star-map mode, the pole of the coordinate system. You can change the upper direction to another pole [(16)]). But you enter "Rotation", you can rotate the image. You can use when you compare a inclaining photo with the image. If the center of the image is Zenith (or the pole of coordinate system), changing "Rotation" makes a complex image. For convenience, I prepare buttons for 8 directions, 9 elevations and "initialize". Direction buttons are written like as "NW", but mean only "NW if Zenithal Coordinate". "initialize" set the center of Projection (to Zenith), Magnitude(<4.5), line of Constellation(ON), the location of the center of Projection in the Image (the Center of the Image), Magnification(=1), Under Horizon(Nothing) and Shape-mode(Nomal). (11)There is the pull down of the list of Constellations(+alpha). You select a constellation and check "Coloring", then the color of the constellation change. If Standard 88 constellation, the color of stars and lines change, but if another, only the color of lines change. The color of Sun, Moon or Planets do not change even if it is selected. If the constellation is under the horizon, the alert appears and the image is drawn usually. You check "Centralizing", then the constellation becomes the center of Projection. In assigned Time mode, the average position of stars over the horizon is calculated. If all stars is under the horizon, the alert appear and the image draw with the old setting of "the center of Projection". In Star map mode, the average position of all stars lighter than mag=5.5 of the constellation is calculated and enter "the Center of Projection". You can centralize to Sun, Moon, or Planets, but you need to set planet-files [(19)]. After drawing, the check of "Centralizing" expires automatically. The coordinate is translated to the coordinate chosen in the drow down of "the Center of Projection", and enter in "Centralizing". If in Zenithal coordinate in assigned time mode, when you change date and time, the coordinate of constellation also change. Thus you must check again if you want to pursue the constellation. On the other hand, if in Equatorial or Ecliptic coordinate, you pursue the constellation without check, even if you change date and time. But If the constellation get under the horizon, the image is black. Sun, Moon and Planets always chage its position even in Equatorial or Ecliptic coordinate. If you want to pursue a planet, you need to check "Centarlizing" at each drawing. (12)You can search by keywords, for example, a star name. Enter keywords and push "Search", then a new window appears and display like Ckick-Search. Up to 9 stars(in the order in Star-Catalogue files). When A star is displayed, the button "Centralize" is enabled. You push the button then the coordinate of the star enters in "The Center of Projection". This searching searchs in All of Star-Catalogue files, so if you enter only numbers, many star are displayed because of coordinate and Magnitude data. ============================================ [D]How to use in a left half in full. (1)There are 3 types of shape of the Main Image. 1-a)Normal Size Square Image of the assigned size. This is for usual Planisphere usage. When you change from other modes to this, automatically "the center of the projection is at the center of the image" is set. 1-b)Half Height The Height becomes the half of the assigned size. When you draw a image around the horizon, you can use all area of the image with the function (14), but the upper side is very skew. Or when you draw All sky in Mollweide projection, for example, Image height is the half of the width. For these reason, I prepare this mode. When you change to this mode, automatically "the center of the projection is at the underline of the image" is set. For using Mollweide projection, set "the center of projection is at the center of the image". Then the center of projection come at the center of the halved height. 1-c)Dual Box All sky is displayed with 2 circles. Each displays a hemisphere. Then the width becomes the double of the assigned size. When you change to this mode, automatically "Magnification=1", "all under the horizon is dispay" and "the center of projection is at the center of image" are set. You can change the setting on "under the horizon". but if you change other settings, the image is broken. (2)When you set a magnification, the image is magnified in the magnification, fixing the center of projection. (Also when you change the position of the center of projection in the image, the center of projection fixed at the position.) you can change "magnification" by the following manners. 2-a)Enter using keyboard. You can enter 7 figures including the point. 2-b)Push "Up" or "Down" button. The step is 0.5 (less than 10) or 1 (more than 10). 2-c)Enter "Scope radius". Assign the angle coresponding to the image from the center to the edge(=(assigned size)/2 pixel), and push "<Mollweide=Azimuthal Equal-Area(0.01093709) >Hammer(0.01010408)>Mercator=Transverse Mercator(0.00984722) =Miller=Sanson=Aitoff=Equirectangular =Azimuthal Equidistant(0.00984697)=Lambert Equal-Area Clyndrical >Stereographic(0.00893112)>Azimuthal Comformal(0.00773399) [The number in () is the square of "(dimension of circle of radius 1degree)/(dimension of main image)" for each projection.] (4)Set "PC's TIME ZONE" to "your PC's TIME ZONE" and "Actual TIME ZONE" to "Your local clock". Usually people don't change TIME ZONE of PC's clock. So usually you don't need to change. But if you change TIME ZONE of your PC's clock, change "PC's TIME ZONE" of this program. The later means, for example: I am in Germany and I set my watch to the local time(CET=UTC+1h), then "Actual TIME ZONE" is also +01h00m. No problem. But I rent a car in Lulea(Sweden, CET=UTC+1h) and go to Rovaniemi (Finland, EET=UTC+2h). Car's clock display CET, but the town clock display EET. Do I do? Only it. (6)Push "OverD" under "DRAW", then the program overdraws the new image on the old image. For example, around a time of a eclipse, you set to display only Sun and Moon, and overdraw at intervals of 10minutes, then the image displays the progress of the eclipse. But the comment area are also overdrawn, so become unreadable. (7)On the window for clicked point 7-a)[dispaying the coordinates corresponding to clicked point] You can change the unit in the window for clicking. You can also change coordinate system to appearent, true, mean or J2000 Equatorial coordinate. (J2000 Equatorial coordinate is always displayed. When you choose J2000 Equatorial coordinate, then J2000 coordinate is doublely displayed.) Instead of searching stars, you can display All coordinate, including Ecliptic coordinates, Greenwich Equatorial coordinate and Local Equatorial coordinate. (in Display Option ->Click and Minute Option [36-d)].) 7-b)[centralizing the clicked point] On the window for clicked point, there is "Centralize" button. You push the button, then the coordinate enter into "the Center of Projection" and the window close. Then you push "DRAW", so the clicked point become the center of Projection. When you push "Centralize", the coordinate is translated in the coordinate system chosen in drop down of "the center of Projection", same as centralizing a constellation. 7-c)[on search by click] When you click the image, the program seachs stars in 1degree from the point, and displays them up to 9 nearest stars in order of angle distance. The window for click displays the following for fix stars: 1st. line:For a star lighter than Mag=5.5, the code of the constellation. In addition, Bayer designation, Flamsteed designation, name, cluster, etc., if there is. For a dark star, only "(a dark star)". 2nd. line:RA and DEC(in the same coordinate system and the unit as 6-a), adjusted on proper motion) and the angle distance from the clicked point. 3rd. line:Information on Magnitude, in the initial setting. (Rmag1, Bmag2, Imag in USNO B1.0 and these average.) For Sun, Moon and planets: 1st. line:the name 2nd. line:RA and Dec(in the same coordinate system and the unit as 6-a), adjusted on geocentric parallax) and the angle distance from the clicked point. 3rd. line:the distance from the observational point, the raidus The angle disntace are measured with or without the annual aberration according as the star. The difference between these cases is max. 1/10,000 (0.36arcs for 1degree, in the case of the direction of Earth-revolving). 7-d)You can change the radius of searching area, but less than 1degree.[Display Option->Click and Minute Option, 36-e)] 7-e)You can change the 3rd. line of the information of a star searched by click, to "the number in the Star-Catalogue" and the average magnitude. "The number in the Star-Catalogue" is original numbering in this system. But I use it in my other program, so I display:-) 7-f)You can search data of "DRAW using FILE"[(35)] same as stars in Star-Catalogues. displayed informations change according to a file and a setting, but position data(RA,DEC) and the distance from the clicked point are displayed always. However the position data is only cut out from the file, not translated in other coordinates. 7-g)[measurement by click] You check "Measure Angle" in the window for clicked point, and you click the image one more time, then the window for clicked point displays the angle distance between two points. (In this time, the program don't search stars.) The window displays the angle in J2000.0 Equatorial coordinate (this is same as in mean or true, Equatorial or Ecliptic) and the angle adjusted the annual aberration, diurnal aberration and the refraction. 7-h)[writing comments at the clicked point] You enter comments in the box of the window for clicked point and push "Comment", then the program write the comments at the click-point. ======================================= [E]Star map mode and Earth map mode (3-b)Star-Map mode You change to Star-Map mode, then the followings change: "Longitude and Latitude" ->"RA and DEC of the Upper Pole", "Date and Time" -> "Epoch", and "Drop down of Coordinate system of Star-Map" and "Shift of Azimuth" are enabled. When you use usual Star Map, you set "The Center of Projection" as the direction that you want to display, and "Magnification", and push "Draw", then the program draw the star map (the upper direction is to the pole of the Equatorial Coordination in default). Remark RA unit is "degree (in decimal)", not "h/m". You can also set by "The Center of Projection" by "Centralizing to a Constellation" same as Assign Time mode. If you don't change the left half, "Zenithal coordinate" equals to "Equatorial coordinate". In the drop down of "The Center of Projection", "Zenital coordinate" and "Equatorial coordinate" is same. Thus it is better that you disable lines of Zenithal coordinate or Equatorial coordinate. When you set "RA and DEC of the Upper Pole", "Zenithal coordinate" become new coordinate system that the pole is assigned RA and DEC. For example, you set RA=270deg,DEC=66.6deg (the pole of Ecliptic coordinate), and the lines of the coordinate coincide with the line of Ecliptic coordinate. But in this condition, "Azimuth=0degree" is the direction to the pole of Equatorial Coordinate (Ecliptic Langitude=90degree). To adjust this slip, you enter 90 degree in "the Shift of Azimuth". Then Zenithal coordinate equals to Ecliptic coordinate. In a same manner, you can make Galactic coordinate. Then, when you set "The Center of Projection", you can choose "Zenithal coodinate=Galactic coordinate", "Equatorial coordinate", "Ecliptic coordinate". You can also set by "Centralize a Constellation". You can choose Zenithal coordinate, Equatorial coordinate (apparent, true, mean, J2000), Ecliptic coordinate(apparent, true, mean, J2000). (Exactly, "J2000 Equatorial" is ICRF. But the difference is less than 0.1arcseconds, you don't need to mind in this program.) "Epoch", diverted "Date and Time", is used for calculation of proper motion. Even if you choose "J2000.0 Equatorial coordinate", Locations of Stars are calculated at Epoch, and displayed in J2000 Equatorial coordinate. And "Epoch" is used for calculation of technical data displayed in the comment area. Also "Epoch" is used for calculation of true or mean Equatorial coordinate and these line. For example, you set "RA and DEC of the Upper Pole"="+180,+90" and the drop down of Star-map mode to true Equatorial coodenate. Then Zenithal coordinate is true Equatorial coordinate, so lines of true Equatorial coordinate and lines of Zenithal coordinate coincide. On the other hand, you display lines of J2000 Equatorial coordinate and lines of Zenithal coordinate, you can draw lines of J2000 and true Equatorial coordinate both. (If you invert it, the same image is drawn.) But you can't see it soon unless the epoch is different more than 100years from AD2000. You also set "Zenithal coordinate" to apparent, true, mean or J2000 Ecliptic coordinate. But inclination of the Earth axis is changing, so you must exactly set it. Galactic coordinate don't change by precession, you set it in J2000 Equatorial coordinate. When you change assigned time mode to Star-Map mode, Longitude, Latitude, time and comment are initialized, but these are recorded in "hayami.ini". When you return assigned time mode, or When you close and reboot, these data are set again. If you change minute options for Click-Window, some of these are not set back to previous conditions. Data in Star-Map mode are not recorded, but you can save a individual file, and load it. (3-c)Earth map mode Before you use Earth map mode, You must prepare map data on a hard disk, and set map data files in "Files" -> "Setting DATA Files". When you change from asigned time mode to Earth map mode, then the followings change as same as to star map mode: "Longitude and Latitude" ->"RA and DEC of the Upper Pole", "Date and Time" -> "Epoch", and "Drop down of Coordinate system of Star-Map" and "Shift of Azimuth" are enabled. When you change from star map mode to Earth map mode, these don't change. In addition, the drop-down of "Selecting Constellation" change from the list of constellation to the list of nations. Units on longitude change from "0 -- 360 degree" to "-180 -- +180 degree" "Date and Time" is set "J2000.0=January 1st AD2000, 12h00mUTC", the base coodinate is set ICRF, "Magnification" is set 4, Magnitude is set 5.5, "the center of Image = the center of the projection", and the coordinate system in Click-Window is set ICRF. You can change these later. But changing the base coodinate and "Date and Time" are meaningless. Oparations are same as in Star map mode. But a sign of longitude is "+ in west, - in east", becase Star map and Earth map are "the reverse" of each other. When you change from Earth map mode to asigned time or star map mode, or v.v., the sign of the longitude in "the Center of Projection" are reversed. =========================================== [F]Projection (13)Select a projection. There are 14 projections and Azimuthal projection defined by user. a)Azimuthal Equidistant projection b)Azimuthal Equal-Area projection c)Azimuthal Comformal prjection(Stereographic projection) d)Gnomonic projection e)Orthographic projection f)Mercator projection(Cylindrical Comformal projection) g)Transverse Mercator projection h)Miller projection i)Equirectangular projection j)Lambert Equal-Area Cylindrical projection k)Mollwaide projection l)Sanson projection m)Hammer projection n)Aitoff projection o)Azimuthal projection defined by user I prepare this projection to reproduce the skew of a photograph. I guess the skew of a photograph is nearly symmetric at the center, so this is Azimuthal. Select "Display Option->Click and Minute Option", then another window appear. Around the center in the window are boxs for the defining polynomial of projection. You must define "the polynomial that the Angle R(rad) from a Point to the Center of projection correponds to the distance R' from the point on the map to the center of the map", and enter the coefficients. This polynomial needs the linear term because of nearly equidistance and comformality. This program fix the coefficient of the linear term to 1, for we compare other projection. For example, Azimuthal Equidistant: R'=R Gnomonic projection: R'=tan(R)=R+R^3/3+R^5*2/15+..... Orthographic projection: R'=sin(R)=R-R^3/6+R^5/120-..... Stereographic projection:R'=2tan(R/2)=R+R^3/12+R^5/120+..... Azimuthal Equal-Area: R'=2sin(R/2)=R-R^3/24+R^5/1920+..... Actual coefficient is decided by "Angle of Scope Radius when magnification=1" and "Magnification". "Angle of Scope Radius when magnification=1" is the angle on sphere corresponding from the center of the image to the edge of the image (i.e. a half of "Size of Image"). In usual planisphere, this is 90degree. For the rest, You enter coefficients of 2 - 9 degree term. A polynomial of 9 degree, so you don't mind divergence, but mind a possibility that this is not monotonically increasing function. It occur like that "Orthographic projection can project only a hemisphere". So you must know the domain in which the function is monotonically increasing. After you enter all coefficients, you push "Check domain", then the program calculate the upper bound that the function is monotonically increasing, and enter the upper bound to "Angle Radius, display in (x1)". You can not draw a map if over the angle. Thus you must enter the angle radius less than the bound. (This calculation is very rough, so the program mistake if coefficients are immoderation.) Then, the coefficients, you decide :-) I have made a few programs to calculate the coefficients from photographs, but these are also complex. Besides, from my feel, it is better that the polynomial is composed of terms of odd degree. The above example is so. If the polynomial contains a term of even degree, Higher derivative of the polynomial make the center discontinuous. When I calculate actually the coefficient from photographs, the polynomial composed of odd degrees only fits more than the polynomial containing even degree. There is one more box, "Aspect Ratio Y/X". Usually this is 1. But on My camera, this is 1.012. So I prepare this box. Remark: When you set the polynomial decided from phtographs very zoomed up and you draw a small magnification, then the program may needs very long time, a few minutes or ten minutes. p)When you assign the Zenith for the center of the Projection, you can draw hemisphare in 4 azimuthal projections, Miller, Equirectangular, Lambert Equal-Area, Mollwaide, Sanson, Hammer and Aitoff projection. But you can not draw hemisphare in Mercator, Transverse Mercator and Gnomonic projection, because hemisphere spreads on a infinte plane. In Star-Map mode, you can not draw all sphere in comformal projections, Gnomonic projection and Orthographic projection. (14)Upper or lower shift of the image When you set the center of projection on the horizon, the lower half of the image become black (white) only, in another word, is not used. So you can shift the image and use all square of image. In "Projection->Set the Position of Direction", You can select the followings: a)the Center of the Image This is the usually usage. b)the Horizon touchs the Bottom When you choose this, the horizon come down to touch the bottom line. This is the efficient usage. But in the case the center of projection go out of the image, the program sets the center of projection on the topline. e)the Center of the Bottom The center of projection come at the bottom line. d)the Center of the Top The center of projection come at the top line. I prepare this to easily compare the image under the Equator and a star map by Mercator or Equirectangular projection. Here, "the horizen" means "Elavation=0degree", does'nt mean the horizon in the view from a high mountain. (15)Display under the horizon In assigned time mode, usually stars under the horizon aren't displayed. But you can display down to 1degree, 2degree, or All. "All" option is mainly for "Dual-Box mode". In Star-Map mode, always All sky is displayed. (16)Direction of Vertical When "Rotation=0degree" in setting "The Center of Projection", you can select the upper direction to "Zenithal pole", "Equatorial pole(true, mean or J2000)" or Ecliptic pole(true, mean or J2000). If you choose "Equatorial pole", the image is just like the view in a equatorial telescope. ===================================== [G]Sun,Moon and Tech (17)You can select to display Sun/Moon as a emphasized circle, a true-radius cicle(painted), a true-radius circle(outline), (x)-marking or not display. When you set a small magnification and true-radius Sun/Moon, it may be difficult that you distinguish Sun/Moon from the Ecliptic line. So it is recommended that you use true-radius Sun/Moon in "magnification>3". Sun is yellow, and Moon is White. (18)You can display the antipode of Sun as (x)-marking or as "the Shadow of Earth". When (x)-marking(simple), (x) comes at the true antipode of the geocentric apparent location of Sun (without the abberation and the geocentric parallax by a distance). When (x)-marking(apparent) or "the Shadow of Earth", you must set the distance from the center of Earth (in the window appearing "Sun,Moon and Tech->planet" [(19)]). The default setting is "the distance to Moon (calculated automatically)". If you set the distance less than the radius of Earth, the program sets the distance as the radius of Earth. Then the program calculates with the abberation and the geocentric parallax by the distance. When "the Shadow of Earth", the program draws outlines of the umbra and the penumbra, made on the hemisphere of the assigned radius with the center same as of Earth. This outlines is calculated with the geocentric parallax. If the assigned distance doesn't make the umbra, only the outline of the penumbra is drawn. When The distance is "the distance to Moon", the radius of the penumbra is roughly same as 5 times of the radius of Moon, so it is difficult to distingish it in a small magnification. When the distance is more than 300,000km, you may first draw (x)-marking, check the location and magnify. The size of Earth-shadow is slightly larger than the size calculated from solid Earth, because of the effect by the atomosphere. You can set the factor in "Planet"-window[(19)]. The default factor is 1.018. When you draw a low sky with refraction-correciton, Earth-shadow is drawn correctly (with the refraction and the skew of projection), but Moon is drawn as true circle proximately. Thus the relation between the Earth-shadow and the edge of Moon is not complete in a low sky. In addition, the Earsh shape in calculating "the Shadow of Earth" is a true ball. Thus there is a errer corresponding to the oblateness of Earth(1/300). (19)You can set the displaying of planets. First you set parameter-files for planets. Next you choose "emphasized circle", "(x)-marking" or "Not display". If you don't set parameter-files and set to display planets, or if parameter-files are incorrect, the program occurs a error and stops. In the same window, you can set the distance from the center of Earth to the Earth-shadow for [(18)]. (20)You can draw a star by assigning the coordinates, in the window of "Sun,Moon and Tech->Star by Location". You check "Adding a Star", then boxes in the window are enabled. You enter RA and DEC and push draw, then you can display the star. The default unit of RA is h/m, but you can change to degree/m. You can also choose the coordinate from Equatorial(apparent, true, mean, J2000), Ecliptic(apparent, true, mean, J2000), or Zenithal. Furthermore, you can choose "Langitude and Latitude of Earth". This is "the above point of the assigned longitude, latitude and distance from Earth", for example, of the position of a satellite or airplain. You can also draw an object on Earth by "Long. and Lat. of Earth". But if the distance between the point of the obsevation and the object is short, You need very high accuracies for the point of the observation and the object. (If a few km, you need "arcsecond(1/1000 degree)"-accuracies or more.) You can draw the star as (x)-marking, circle(painted) or circle(outline). When you choose drawing as circle, you assign the size from "Magnitude" or "radius(degree)". It is better that you set "Magnitude" lighter more than the actual, so you can see easily. When you check "Distance", you can enter a distance (from the center of Earth or the surface of Earth). The unit is "AU"or "km". Then the program calculate the geocentric parallax. If you draw an object on Earth, you check "From the surface" and enter the altitude in the same geodetic datum as for the point of the observation. When you choose "distance from the center of Earth", the program calculates as the star is the RA, DEC and the distance from the center of Earth". Thus, If you set the function of displaying the coordinate[(22)] in the same coordinate system, the displayed coordinate coincides with the coordinate you enter. (In Zenithal coordinate, these coincides without adjusting diurnal aberration and refraction.) When you choose "distance from the surface of Earth", the program calculates as the star is the RA, DEC and the distance from the point of obserbation, except "Longitude and Latitude of Earth". Thus if you set the function of displaying the coordinate[(22)] with geocentric parallax, the displayed coordinate coincides with the coordinate you enter. (In Zenithal coordinate, these coincides with adjusting diurnal aberration and refraction.) When you choose "distance from the surface of Earth" and "Longitude and Latitude of Earth", the program calculates as the star is at the distance directly above the RA, DEC of the surface of Earth. Thus the coordinate you enter and "Greenwich Equatorial coordinate with geocentric parallax" don't coincide. When you enter the box "Name", it is displayed in the comment area, (In assigned time mode, it is displayed when the star is over the horizon). After drawing, you can overdraw any times with changing coordinates, by pushing "OVERD". But when you push "DRAW", this function can draw only a star. Data in this window can be saved and loaded. The extension is ".str". (21)You can assign orbital elements of object and draw the position calculated from the elements. a)You choose "Sun,Moon and Tech->Object Defined by Orbit ->Orbital elements", then the window for orbital elements appear. b)you choose "around Sun" or "around Earth". The unit of distances is "AU" when "around Sun", "km" when "around Earth". Next you choose "Perihelion Passage" or "Epoch and Mean Anomaly". When "Perihelion Passage", the box of "Mean Anomaly" is disabled and fixed to "0". Next you choose "arguement of Perihelion" or "Longitude of Perihelion". c)There are 4 box for distances. But if eccentricity less than 1, two distances in "Perihelion Distance", "eccentriciy","Semi-major Axis or Period" decide others. You enter 2 distance and push "Calculate", then the program calculate and enter others. If you enter 3 or 4 distances, the program calculate from "Perihelion Distance" and "eccentriciy" to "Semi-major Axis", and next to "Period". If eccentricity is 1 or more, "Semi-major Axis" and "Period" become "***.***". d)You enter other boxes. e)You can save and load these data. f)You push "OK", then the window closes. g)You choose "Emphasized" or "(x)". You push "DRAW", the program calculate the location of the assigned date and draw. This calculation is a simple Two-body calculation, So low accuracy. Use as a prediction in short time or a rough estimate. (22)Though Sun and Moon are displayed in Image, Azimuths and Elavations of Sun and Moon, and Sky Condition (Daylight, Twilight, Astoronomical Twilight, night) are displayed on the comment area in assigned time mode. In addition, You can display coordinates of Sun, Moon, planet or object in "Sun,Moon and Tech" in selected coodinate system. You can select the following option: Object:Sun,Moon,planet,"Star by Location","Object defined by orbit" Observational place:"from geocenter"(default) or "with geocentric parallax" Condition of aberration:"apparent" (calculating with annual aberration), "No annual abberation" (eliminating annual aberration) or "Infinite Light Speed" (eliminating planet aberration) Coordinate system:Equatorial(J2000 ,mean, true, Greenwich, Local), Ecliptic(J2000, mean, true, Greenwich, Local) Zenithal In usual books, "apparent Equatorial(Ecliptic)" means "geocentric apparent true Equatorial(Ecliptic)". On the other hand, "true(mean/J2000) Equatorial(Ecliptic)" in usual books means "geocentric, no annual aberration, true(mean/J2000) Equatorial(Ecliptic)". When "with geocentric parallax", "apparent" and "Zenithal coordinate", the program calculate with diurnal aberration and refraction (when assigned respectively). When You change to Zenithal coordinate, "with geocentric parallax" and "apparent" are set automatically, but you can change. Even if you choose any setting, the location in the image and the default display on Sun and Moon in comment area are the apparent location with geocentric parallax. Instead of displaying coordinates, you can display the digression from Sun to a object you select. If you choose Sun or Moon as the object, the digression from Sun to Moon is displayed. In this case, the following are displayed: "the defference of Longitude from Sun to the object" "the defference of Right Ascension from Sun to the object" "the true angle between Sun and the object" "the Angle of the north pole - the object - Sun" "the Angle of the Zenith - the object - Sun" The directions in the last two angle are conter-clockpwise from "the north pole or the Zenith=0 degree". These data contain calculations on "Obsevational Place" and "Condition of Location", but do not contain calculations on diurnal aberration and refraction. (23)You can display data for the precession and the nutation. You can choose "North pole and Equinox" in "mean or J2000 Equatorial coordinate" or "Ecliptic pole and Equinox" in "J2000 Ecliptic coordinate". You can also display data of the Nutation, Aberrations or Sidereal Time. (24)You can change units in (22) and (23) [36-b)]. But the default display on Sun and Moon (degree in decimal) are not changed. Remark for Comment Area: You can select to display or not to display "data on the location of Object","Comment of Adding a Star", and "Precession and Nutation" respectively. When you choose all, these are displayed in the order of the above. But if "Size of Image" is small, some data are out of the image. If "Size of Image<248", a part of default comments are out. If "Size of Image>516", all are displayed. =================================== [H]Display (25)you can choose "stars are white, the background is black" or "stars are black, the background is white". (26)You can choose How light star are displayed. You can choose "all stars are not displayed". (26-a)Scaling a star The default radius of a star in the image is (7.5-"Magnitude")*sqr("Size of Image"/1000). You can change the part of "7.5" and the factor for the entirety (the default settings are "7.5" and "1"). This numbers are saved in "hayami.ini" when the program is closed. (27)You can shoose "lines of constellations is displayed or not". But If you check "Coloring of a Constellation", the selected constellation are displayed even if you choose "not display". (28)You can choose display lines of Zenithal coordinate, Equatorial coordinate or Ecliptic coordinate. Respectively, you can set the interval of 5degree, 10degree, 30degree, 90degree, only horizon/equator/ecliptic or nothing. In Zenital coordinate, "Horizon" is "elavation=0degree". When a low altitude, "true horizon"(the skyline you van observe) is overdrawn over "Elavation=0degree". But when a high altitude, both "true horizon" and "Elavation=0degree" are drawn separately. In Equatorial coordinate and Ecliptic coordinate, "apperant" is default setting, but you can change to "true", "mean", "J2000.0" respectively. When you set "Numbering" on, the numbers are written for each lines. In principle, the numbers are written around the fringe of the image or under the horizon(in assigned time mode). But, for example, in the case of lines around a pole in a low magnification, the lines don't touch the fringe nor the horizen, so the numbers are written in the image. Sometimes, a number for RA and a number DEC may be overwritten. (29)You can draw the line of Moon. "the line of Moon" always changes and has very large geocentric parallax. Thus 4 type of moon lines are prepared. a)Mean Orbit calculated from 2 degree-polynomials, b)Apparent c)with Parallax 1 d)with Parallax 2 a) is the great circle drawn with 2 degree polynomial for the asending node and the constant inclanation of Moon. The difference from b) around the assigned time is 10 arc-minutes or so for latitudes, but the difference around the antipode is larger. b) is "apparent points from 15 days before to 15 days after the assigned time, without geocentric parallax". The line for 30 days, so this overlaps around the antipode, with a slight slipping. This needs calcualtions of Moon location for 30 days, so needs many times. c)"with Parallax 1" is "apparent points from 15 days before to 15 days after the assigned time, with geocentric parallax from the assigned latitude and local sidereal time". Though "the observatorial point" is not the geocenter, it is a fix point in the celestial grobe. If the line drawn at "Tokyo 21h" runs over the Pleiades, there is a location of the same latitude as Tokyo (35.7degree N) from witch a occultation of the Pleiades can be seen around 21h. d)"with parallax 2" is "apparent points from 15 days before to 15 days after the assigned time, with geocentric parallax from the assigned point". This is affected by the Earth rotation, thus this line waves. These points are observed from a fixed point, but includes "points under the horizon". Then the program draw the line with white for "parts over the horizon" and with blue for "parts under the horizon". If a white part of the line run over the Pleiades, a occultation of the Pleiades can be seen from the assigned point (though the occultation may occur at a midday.) (30)You can draw the lines of Longitude and Latitude of Earth, in Assign time mode. But when a low altitude, you can't see well. Use this function when "altitude>2000". When you set "Altitude of Lng. and Lat. Line" in [36-c)], the program draw lines of longitude and latitude in the assigned hight. You can use to check clouds, airplanes or satellites. The program uses GRS80 as the reference ellipsoid in calculation, but the difference from WGS84 is small. Numbering for lines of longitude and latitude are not prepared. If you need, You draw a point by "Star by Location" in "Lng&Lat of Earth", entering proper longitude, latitude and distance. In other setting of "Star by Location", a star under the horizon is not display, but in "Lng&Lat of Earth" the point is display. (31)Scale of the Coordinate originated from the Projection Center You can draw scales of the Coordinate originated from the Projection Center. The interval of scales is decited as it become larger than 36pixel. This is used mainly in a large magnification. Types of scale are a)a vertical line and a horizontal line b)coordinate like as "Long:0deg,Lat:0deg" on Earth c)coordinate rotated 90deg from b) d)polar coordinate. (32)"Refraction Correction" is calculated in default. But you can set not to calculate it. Approximation of Refraction is applied to 2degree under horizon. (33)"Diurnal Aberration" is calculated in default. But you can set not to calculate it. (34)You can select How to calculate "Centralizing a Constellation". Options are followings: Simple:Simple Average of the location of stars lighter than Mag=5.5 lines :Average with weightening stars relating to lines of the constellation Magnitude:Average with weightening by "6-(Magnitude)". These are much same. But in "lines" option, the program reads the file of lines. When the file of lines is too large, you avoid "line" option. (35)"DRAW using FILE" You can draw with another file. You can also search by click same as star-catalogues, or search by keyword. This function is very complex, so I don't explain now. If you have "ngc2000.dat", read "on_ngc.txt". (36)"Click and Minute Option" a)You can set the radius of a star in the image according to the Magnitude [26-a)]. This radius is applied to "Emphasized circle" of "Star by Location". b)You can set the units of Sun, moon and Tech's information in the comment area [(24)]. c)You can set the altitude for line of Long.&Lat. of Earth [30)]. d)You can set units of Azimuth,Elavation and RA,DEC respectively, in the window of click. You can choose the followings: degree in decimal(RA or Longitude are -180 to +180) degree in decimal(RA or Longitude are 0 to 360) degree in sexagesimal(RA or Longitude are -180 to +180) degree in sexagesimal(RA or Longitude are 0 to 360) h/m/s for RA or Longitude(degree in Sexagesimal in DEC or Latitude) You can also choose the unit of refraction in the window of click from degree in decimal or sexagesimal. But for "DRAW using FILE", data are displayed from the file directly, so you can not change units of these data. You can select RA,DEC in the window, from "apparent", "true", "mean" and "J2000". RA,DEC in J2000 are always displayed, so RA,DEC in J2000 are displayed double if you choose "J2000". You can chage from seacrhing by click to displaying all of Equatorial(Local,Grennwich,apparent,true,mean,J2000) and Ecliptic(apparent,true,mean,J2000). e)You can set the radius for searching by click, but less than 1degree. If you enter more than 1degree, the program searchs in 0.99999degree. You can also change informations desplayed in the window for searching by click [7-e)]. =================================== [I]File (37)You can save and load data of Observational location, i.e. Longitude, Latitude, Altitude, actual TIME ZONE and comment. The extension is ".ini". When in star-map mode, you can save and load data of coodinate system, i.e. RA and DEC of the Upper Pole, Shift of Azmuth and comment. The extension is ".crd". (38)You can save the image as bitmap. (39)In "File-> Setting DATA Files", You can set 1st. Star Catalogue(lighter than Mag=5.5), 2nd. Star Catalogue(darker than Mag=5.5), the file of line data of Constellations(in Coordinate) the file of Constellation's name, the file of data of Cities, (a reserving box, you set "zentend.txt",dummy data), the file of line data of Coast and Boundary, the file of Nation's name. a)You can change other star-catalogues with same format. But 1st catalogue has data relating some functions. 2nd catalogue has only RA, DEC and Magnitudes. b)You can make the file of line data of Constellations with cnatlnet.exe. c)You can make the file of Constellation's Name. But First 3 letters in each line are related to selecting a constellation (Coloring, Centralizing, Search by click), so you must match these. d)You can also change the setting for language. This setting is applyed to Constellation's name and comment. The font is "Arial" or "Courier New" in Europian language, "MS UI Gothic" or MS Gothic in Japanese. But if the version of MS-Windows and this setting are mismatched, letters may be displayed incorrectly, for exsample in drop-downs or box. Constellation's name in the image and the window for click are displayed correctly, perhaps. But if comment doesn't enter correctly, the incorrectness may be reflected in the image. If "MS UI Gothic" doesn't exist, the program uses "Arial" and "Courier New". (except Constellation' name and comment, "Arial" or "Courier New" are used). But this font-setting are separated from the setting the file of Constellation's name. So you must match these. (40)"End" You can end here. =============================================== [J]Error on Operation 1)When you close the program in Star-Map mode, settings changed in Star-Map mode are not saved in "hayami.ini". For example, You change a file of constellation's line ->You change to Star-Map mode (Here "hayami.ini" is saved.) ->You change a file of constellation's line ->You close ("hayami.ini" is not saved) Then the second change are not saved. 2)The program takes very long time if you choose many heavy options, especially Azimuthal projection defined by user in low magnification. 3)Sometimes, the program may mistake to save locations of windows. Then you can not find the window (maybe the window go out of your monitor). If it occurs, delete or correct "hayami.ini". (line 1 and 2 are the location of the main window, line 3 and 4 are the location of the image window, line 26 and 27 are the location of the window for click and search.) If you delete, the program uses the initial setting written in the program. When you close badly, the program intercepts writing "hayami.ini". Then the program stops with error when you reboot. In this case, delete "hayami.ini" [K]Technical matters (a)Locations of fixed stars are read from Star Catalogues in ICRF. And the proper motion, precession, nutation (terms with sings more than 0.01arcs), annual aberration aplied. Diurnal aberration and refraction are aplied when you choose these and assigned time mode. (The order of calculations may be changed, but mathematically same except errors by rounding). Annual parallax and polar motion are not aplied. For Sun, Moon and planets, geocentric parallax is aplied. planet aberration is "recalculation one more time". Because of ignoring the relativity and deference of orders of calculations, there is a small difference between planets location data in Comment Area and planets location data in the click-window. For "Star by Location" and "DRAW using File", the program translates from assigned coordinate system to the apparent position, and geocentric parallax, diurnal aberration and refraction are aplied if you choose these options respectively. (b)The parameters of procession are described in "prmprc.txt" as polynomials of max. 6 degree. But This is "3-1-3-1 matrix form", not "1-3-1 matrix form" same as IAU76. (Williams,AJ,108(1994),pp711-724 and Fukushima,AJ(2003),pp494-534) (c)"Date and Time" is treated as UT1 or UTC, but the program translate to ET/TD internally. Before AD1600, the program uses approximate polinomial of 2degree. After AD1600, the program reads and uses "ET-UTC.txt". After AD1958, (TAI)+32.184s are used in effect. If a leap second is inserted, correct "ET-UTC.txt". =================================== [L]Reference Star-Catalogue:USNO B1.0,the United States Naval Observatory, Flagstaff Station (http://www.nofs.navy.mil/data/fchpix/) Constellations containing stars,lines of Constellation: Field Star Map2000(Seibundou-Shinkousya) Astronomical Annual 2007(Seibundou-Shinkousya) Name of Constellation(Japanese and Latin),Abbreviation of Constellation: Astronomical Annual 2007(Seibundou-Shinkousya) Names of Constellation(English):"Kenkyusha Readers+plusV2"EP-WING CDROM version(Kenkyusha) Names of Constellation(German,Franch,Italian,Dutch):Wikipedia(each langage) Bayer designation,Flamsteed designation,Names of stars: Annual of Science 2004,(National Astronomical Observatory of Japan,Maruzen) Field Star Map2000(Seibundou-Shinkousya) Astronomical Annual 2007(Seibundou-Shinkousya) Wikipedia(English,German) Projection of Map:T.G. Feeman, "Portraits of the Earth, A Mathematician Looks at Maps", Mathematical World Volume 18, American Mathematical Society, Wikipedia(English,Japanese) Shape of Earth:Annual of Science 2004,(National Astronomical Observatory of Japan,Maruzen) Calculation for Positions of Astronomical Object,(Kou Nagasawa,Chijin-shokan) Greenwich mean sidereal time at 0hUTC: Annual of Science 2004,(National Astronomical Observatory of Japan,Maruzen) Relation on UT and ET or TD:L.V.Morrison and F.R.Stephenson, "Historical Value of the Earth's Clock Error dT and the Calculation of Eclipses",JHA2004, Annual of Science 2004,(National Astronomical Observatory of Japan,Maruzen) http://jjy.nict.go.jp/mission/page1.html Location of Sun, Moon:the Extension to increase periodical terms and to get the precision high, of the equation of Japan Coast Guard(1978,1980), fitted to JPL-HORIZONS(http://ssd.jpl.nasa.gov, DE405+DE406). Mean Elements of planets:J.L.Simon, P.Bretagnon, J.Chapront, M.Chapront-Touze, G.Francou and J.Laskar,"Numerical expressions for precession formulae and mean elements for the Moon and the planets", Astron. Astophys. 282,663-683(1994) Precession:T.Fukushima,"A New Precession Formula",AJ126(2003),pp494-534 Nutation:T.Shirai and T.Fukushima,"Construction of a New Forced Nutation Theory of the Nonrigid Earth",AJ121(2001),pp3270-3283 Aberrations:Calculation for Positions of Astronomical Object,(Kou Nagasawa,Chijin-shokan) (but I change from using rotation matrice to adding vectors and normalizing) Refraction(base data):Astronomical Annual 2007(Seibundou-Shinkousya) Two body calculation(in "Object defined by orbit"): Calculation for Positions of Astronomical Object,(Kou Nagasawa,Chijin-shokan) Longitude, Latitude and Altitude of cities of Japan: Chorographic map 1:200,000[Image data in CD-ROM and MAPDSP3.2] (Geographical Survey Institute of Japan) Longitude, Latitude and Altitude out of Japan: Topographic maps by authority on Land-Survey in each country, Wikipedia(mainly English version),or others Programing Longuage:F-BASIC V6.3L10 U0003(Fujitsu) =================================== [M]History Jul 24th,2007:checked by one of my friend [-omission-] Apr 24th,2009:Renewal on the interface of the main window, changing the format of .plt files, external file for the nutation. May 15th,2009:The parameter-file for Saturn(temporary), increasing item saved as ".str", increasing numbers of figures for longitudes and latitudes of "The place of Sight" and "Star by the location", Adjusting the layout of the main window. Jun 05th,2009:Adjusting treatments on "Additional Constellations", Changing the number-displaying from "rounding toward 0" to "Round Half Up", strdrt.exe Jun 12th,2009:changing calculations and options on the antipode of Sun, writing Comments at a ckick-point, changing the layout of the window for click. Jun 17th,2009:adding new items of "Moon line", adjusting lines of longitudes and latitudes. Jul 05th,2009:Changing orders of calculation on geocentric parallax, adjusting names of planets, changing the accuracy of click-search, adjusting display of numbers(especially number less than 1degree), adjusting the index, adjusting the size of the click-window, changing options of displaying Location data of planets, adding planets to objects in click-search, display the radius of planets in the location data, calculating abberations of the ojbect assigned by orbital elements. Jul 24th,2009:the Factor of "Shadow of Earth", adjusting lines of "Shadow of Earth", Centralizing to Sun, Moon or Planets, Scales of Rectangular Coordinate. Jan 22nd,2011:Coordinate lines originated from the center of the projection, Marking at the click-point, Marking when the result of keyword-seach is unique, saving the coordinate system in Click-Window to "hayami.ini", setting autmatically to ICRF when choosing Map-mode, changing the display-style of search by click or keyword ====================== ftcenter@mth.biglobe.ne.jp http://www2s.biglobe.ne.jp/~ftcenter January 22nd, 2011.