CN106055700A - Infrared band flux expansion calculation method based on infrared star catalogue - Google Patents
Infrared band flux expansion calculation method based on infrared star catalogue Download PDFInfo
- Publication number
- CN106055700A CN106055700A CN201610430215.6A CN201610430215A CN106055700A CN 106055700 A CN106055700 A CN 106055700A CN 201610430215 A CN201610430215 A CN 201610430215A CN 106055700 A CN106055700 A CN 106055700A
- Authority
- CN
- China
- Prior art keywords
- star
- wave band
- luminosity
- flow
- star catalogue
- Prior art date
- Legal status (The legal status is an assumption and is not a legal conclusion. Google has not performed a legal analysis and makes no representation as to the accuracy of the status listed.)
- Granted
Links
Classifications
-
- G—PHYSICS
- G06—COMPUTING; CALCULATING OR COUNTING
- G06F—ELECTRIC DIGITAL DATA PROCESSING
- G06F16/00—Information retrieval; Database structures therefor; File system structures therefor
- G06F16/20—Information retrieval; Database structures therefor; File system structures therefor of structured data, e.g. relational data
- G06F16/24—Querying
- G06F16/245—Query processing
- G06F16/2458—Special types of queries, e.g. statistical queries, fuzzy queries or distributed queries
- G06F16/2465—Query processing support for facilitating data mining operations in structured databases
-
- G—PHYSICS
- G06—COMPUTING; CALCULATING OR COUNTING
- G06F—ELECTRIC DIGITAL DATA PROCESSING
- G06F16/00—Information retrieval; Database structures therefor; File system structures therefor
- G06F16/20—Information retrieval; Database structures therefor; File system structures therefor of structured data, e.g. relational data
- G06F16/22—Indexing; Data structures therefor; Storage structures
- G06F16/2282—Tablespace storage structures; Management thereof
Landscapes
- Engineering & Computer Science (AREA)
- Theoretical Computer Science (AREA)
- Databases & Information Systems (AREA)
- Physics & Mathematics (AREA)
- General Engineering & Computer Science (AREA)
- Software Systems (AREA)
- Data Mining & Analysis (AREA)
- General Physics & Mathematics (AREA)
- Probability & Statistics with Applications (AREA)
- Computational Linguistics (AREA)
- Mathematical Physics (AREA)
- Fuzzy Systems (AREA)
- Photometry And Measurement Of Optical Pulse Characteristics (AREA)
- User Interface Of Digital Computer (AREA)
Abstract
The invention belongs to the field of space-based and ground-based photoelectric observation, and discloses an infrared band flux expansion calculation method based on an infrared star catalogue. The method comprises the steps of selecting a known infrared star catalogue, screening target sources satisfying demands, and extracting corresponding parameter items; calculating infrared colour indexes of all target sources in an expansion star catalogue, and carrying out classification based on colour index parameters; converting star magnitudes of four bands in the expansion star catalogue into flux based on isophotal frequency based on isophotal wavelength and isophotal flux method; determining a flux fitting function of each start in the expansion star catalogue; fitting a function according to continuous spectrum of high-precision spectrum of a Vega, determining isophotal wavelengths and isophotal frequency of expansion bands in the expansion star catalogue, and the corresponding isophotal flux expressed by wavelengths and frequency of the bands; obtaining the flux value of each target source of the expansion star catalogue in the expansion bands; and determining the star magnitudes of the target sources of the expansion star catalogue in the expansion bands by taking the flux of the Vega in the bands as flux zero points.
Description
Technical field
The invention belongs to space-based and ground photoelectric observation field, relate to a kind of infrared band flow based on infrared star catalogue and open up
Exhibition computational methods.
Technical background
Along with China's ground-and air-based is in the development of infrared band Detection Techniques, in the urgent need to China's autonomous device work
The infrared star catalogue of high accuracy that wave band is consistent, provides the calibration of high-precision flow, positions and sensing etc. being embodied as autonomous device
Hold.At present existing the most multiple (include WISE, Spitzer of the U.S., and the AKARI of Japan based on infrared space telescope
Deng) the infrared star catalogue that obtains, but because the difference of scientific goal, each space telescope has the service band of oneself uniqueness, because of
This, the star catalogue of formation also comprises only the infrared magnitude information of its particular job wave band corresponding.The autonomous infrared equipment of China is gathered around equally
There is the service band of oneself uniqueness, be difficult to find that applicable Chinese Space and the calibration of ground based IR equipment specific band the most in the world
The near-infrared required with orientation etc. and mid-infrared star catalogue.
Summary of the invention
This method mainly for be difficult to find that in the world at present applicable China particular space or the calibration of ground based IR equipment and
Near-infrared needed for orientation etc. and a difficult problem for mid-infrared specific band star catalogue, propose based on existing infrared star catalogue by waiting luminosity ripple
High accuracy expansion that is long and that wait luminosity method of flow and high-precision classification approximating method to realize infrared band, thus generate infrared
The high accuracy star catalogue of meaning wave band.The present invention can build and by the design wave band of the space built and ground based IR equipment according to China
Requirement, provides the high accuracy infrared star catalogue consistent with design wave band for it, thus realizes exact flow rate calibration for it, position and refer to
To providing powerful guarantee.
The present invention is realized by below scheme:
A kind of infrared band flow based on infrared star catalogue expands computational methods, and described method is by existing known red
Outer star catalogue is as fundamental catalog, by waiting luminosity wavelength and waiting luminosity method of flow and classification approximating method
Realize the expansion of infrared band, generate the star catalogue of infrared any wave band, the star of described infrared any wave band
Table is for expanding star catalogue, and described method comprises the steps:
Step one: selection known infrared star catalogue, screens satisfactory target source, extracts relevant parameter item；
Step 2: calculate the infrared colour index of all target sources in described expansion star catalogue, and based on parameter essences such as colour indexs
Really classification；
Step 3: based on waiting luminosity wavelength and waiting luminosity method of flow to be converted into expanding the magnitude of four wave bands in star catalogue
Based on the flow waiting luminosity frequency；
Step 4: determine the flow fitting function of every star in described expansion star catalogue；
Step 5: according to the continuous spectrum fitting function of Vega high accuracy spectrum, determines that Vega is opened up in expanding star catalogue
Exhibition wave band wait luminosity wavelength, etc. luminosity frequency and correspondence thereof this wave band respectively with wavelength and frequency representation etc. luminosity stream
Amount；
Step 6: in acquisition expansion star catalogue, each target source is at the flow value expanding wave band；
Step 7: with Vega at the flow of this wave band for flow zero point, it is thus achieved that in described expansion star catalogue, each target source exists
Expand the magnitude of wave band.
Further, described step one specifically includes:
(1) based on required expansion wave band and the sky distribution situation of target source, investigate and select applicable
Know infrared star catalogue, be used as the fundamental catalog expanded；
(2) fundamental catalog coordinate and each infrared band magnitude are screened, select required four wave bands in fundamental catalog
The target source of at least 3 wave band effectively observations, is formed and expands star catalogue；
(3) coordinate and the known infrared magnitude important parameter item of each four wave bands of target source in expansion star catalogue are extracted, described
Four wave bands represent with W1, W2, W3 and W4 successively from being short to length.
Further, described step 2 specifically includes:
(1) infrared colour index W1-W2 of all target sources, W2-W3 and W3-W4 in expansion star catalogue is calculated；
(2) to expand W2-W3 colour index in star catalogue as main criterion, W2-W3 colour index is as secondary criterion, to expanding star
All target classifications in table, are divided into 16 subclasses；
(3) to meet main criterion with time criterion as condition simultaneously, four wave band flow zero point phases described in each target are selected
Answer correction factor fc, carry out flow zero point correction by affiliated subclass described four wave bands corresponding to each target；
(4) according to judged result, adding a columns in expanding star catalogue, to record judged result, described row are named
color_n；Described color_n row numerical value be a, a be integer.
Further, described step 3 particularly as follows:
To expand in star catalogue, the numerical value of color_n row is as criterion, by four wave band W1 described in expansion star catalogue, W2, W3, W4
Magnitude is converted into based on the flow waiting luminosity frequency；
If color_n meets 1 color_n 4, then W1, the formula of the luminosity flows such as W2, W3 calculating is:
The formula of the luminosity flows such as W4 calculating is:
If color_n is unsatisfactory for 1 color_n 4, then use calculates W1, the luminosity flow such as grade of tetra-wave bands of W2, W3, W4
Formula be formula (1)
Wherein X=1,2,3,4；
For certain star fundamental catalog WX wave band with frequency representation wait luminosity flow, unit is Jy；
FV(iso)WXFor WX wave band Vega with frequency representation wait luminosity flow, unit Jy；
For this star of WX wave band with the correction factor of the flow zero point of frequency representation, dimensionless；
mWXFor this star at the WX wave band magnitude of fundamental catalog.
Further, described step 4 specifically includes:
The value of color_n in expansion star catalogue, as criterion, determines and expands the flow fitting function of each star in star catalogue, and
Determining the coefficient of correspondence of functional equation, the value of color_n is integer, and we are according to the value of color_n, and point three kinds of situations process
(1) when the integer that color_n is satisfied-3≤color_n≤4 condition, this star streaming amount and frequency with one three times
Spline-Fitting；Described cubic spline function refers to be the function of cubic polynomial in each minizone；
(2) when color_n is the integer meeting 100≤color_n≤1131 condition, the fitting function of this star streaming amount
For:
FVFor flow, unit Jy, obtain from step 3 calculates；V be each wave band of WISE etc. luminance frequency, unit
Jy；A and b is constant coefficient, the value of a equal to the value of color_n, b by input front 3 wave bands of WISE in formula (3) and
Flow is tried to achieve；
(3) when color_n is " NULL ", illustrated that corresponding wave band magnitude data is abnormal, this star streaming amount wouldn't have been appointed
Where is managed.
Further, described step 5 specifically includes:
(1) because wouldn't clearly expand each wave band relative spectrum response RSR situation of scope, temporarily in terms of each wave band RSR=1
Calculate, therefore take centre wavelength for waiting luminosity wavelength；
(2) luminosity flows such as expanding this wave band corresponding to wave band is obtained；
Based on formula (4). try to achieve the luminosity flows such as Vega monochromatic flux at the luminosity wavelength such as correspondence, i.e. this wave band
vFV=λ FλFormula (5)
Obtain the described expansion wave band luminosity flow such as grade with frequency representation
(3) the luminosity frequency such as grade of described expansion wave band is obtained according to formula (5)
FλFor luminosity flows such as wave bands；FV(iso) it is the wave band luminosity flow such as grade with frequency representation；ν (iso) is to wait luminosity
Frequency；λ (iso) is to wait luminosity wavelength；ν (iso) unit Hz, FV(iso) unit Jy, λ (iso) unit μm, c=2.99792458
×1014μm s‐1,Fλ(iso) unit W cm-2μm‐1, it is adaptable to 2.5 < λ < 29 μm.
Further, described step 6 specifically includes:
Step 5 obtained expands fitting function and the public affairs expanding the luminosity frequency substitution step 4 such as wave band described in star catalogue
The formula (4) of formula (3) and step 5, obtains expanding in star catalogue each star at the flow value of described expansion wave band, described flow value with
Jy is unit.
Further, described step 7 specifically includes:
Step 6 obtained expands zero etc. that each star in star catalogue obtains at the flow value of described expansion wave band and step 5
Star substitutes at the luminosity flow value that waits of described expansion wave band
Wherein, FV(iso)sourceFor the luminosity flow value such as grade of described expansion wave band target source, FV(iso)0For described expansion
The luminosity flow value such as grade of zero star such as grade (i.e. Vega) of wave band.
Obtain and expand the magnitude that each star in star catalogue is flow zero point at the flow with Vega of a certain expansion wave band, and use
Similar method obtains expands other expansion wave band magnitudes of star catalogue, completes to expand star catalogue.
Further, described fundamental catalog is U.S. WISE space telescope whole day source of release table.
Technical scheme compared with prior art has the following technical effect that
(1) the luminosity method of flow such as the employing of the present invention realizes the expansion to infrared band, compared to whole waveband integral
Deng additive method, guarantee to expand also have under accurate premise computing faster with waveband selection feature more flexibly.
(2) present invention uses sophisticated category to fundamental catalog, have employed accurate and only to each wave band of each classification
Special zero point correction, the Energy distribution of each wave band of classifying difference have employed different fitting functions.Present invention employs based on
The sophisticated category method of infrared color index, for WISE star catalogue own characteristic, obtains 16 kinds of effective classification altogether, and to each class
Not each wave band has carried out different zero point corrections, additionally, the different Energy distribution classifying each wave band have employed different matchings
Function, these ensure that the accuracy of expansion.
(3) present invention has preferable expansion.The present invention covers the most full WISE with current near-infrared and mid-infrared sky
Star catalogue is fundamental catalog, realizes the covered minimal wave length of WISE and in long wavelength range and neighbouring appointing based on this fundamental catalog
Meaning infrared band high accuracy is expanded.But the fundamental catalog of this method is not limited in WISE star catalogue, it is possible to extend to other infrared
Star catalogue, even optics or its all band star catalogue, thus realize the expansion of any wave band.
Accompanying drawing explanation
Fig. 1 is high accuracy infrared band expanding method based on the infrared star catalogue research flow chart of the present invention.
Detailed description of the invention
A kind of infrared band expanding method based on infrared star catalogue, said method comprising the steps of:
Step one: selection known infrared star catalogue (WISE star catalogue), screens satisfactory target source, extracts relevant parameter item
(1) based on required expansion wave band and the sky distribution situation of target source, investigate and select applicable known infrared star
Table, is used as the fundamental catalog expanded, as realized U.S.'s WISE space telescope (astronomical satellite) that whole day observation covers at present
Whole day source of release table (hereinafter referred to as: WISE star catalogue)
(2) fundamental catalog coordinate and each infrared band magnitude are screened, select satisfactory target source, formed new
Expansion star catalogue (hereinafter referred to as " IR-TZ star catalogue ")；
(3) to expanding each target source extraction coordinate and known infrared magnitude in star catalogue, (four wave bands are used successively from being short to length
W1, W2, W3, and W4 represents) important parameter item；
Because observation condition is limited, in fundamental catalog, partial target source only has certain 12 wave band in 4 wave bands to be seen
Surveying, the wave band not being observed can be labeled as NULL, and the significant wave segment data target source less than 3 is mainly rejected in screening.Certainly,
According to fundamental catalog selected by reality and the wave band situation being actually needed expansion, reject other numerical value limited within the most optional 3.
Step 2: calculate and expand the infrared colour index of all target sources in star catalogue, and accurately divide based on parameters such as colour indexs
Class
(1) calculate the known infrared colour index of all target sources in IR-TZ star catalogue, for (W1-W2) in WISE star catalogue,
(W2-W3)、(W3-W4)
(2) using " colorw23 " (i.e. the W2-W3 colour index) in IR-TZ star catalogue as main criterion, " colorw12 " (i.e.
W2-W3 colour index) as time criterion, to meet main criterion with time criterion as constraints simultaneously, to mesh all in IR-TZ star catalogue
Mark classification, is divided into 16 subclasses.
(3) WISE each wave band flow zero point correction factor fc of different subclasses is different, meets main criterion when simultaneously
During with secondary criterion, by affiliated subclass, each target correspondence WISE corresponding correction factor of each waveband selection is carried out flow zero point and repair
Just, correction factor is shown in Table 1.
(4) according to judged result, IR-TZ star catalogue adds the row of entitled " color_n " (its value is integer), with record
Judged result, note " color_n " value be a, a be integer.
Tetra-wave band flow zero point correction factor tables of each subclass of table 1 each target correspondence WISE
Step 3: based on waiting luminosity wavelength and waiting luminosity method of flow to turn expanding the magnitude of tetra-wave bands of WISE in star catalogue
Turn to based on the flow Fv (iso) waiting luminosity frequency v (iso)
With the value of " color_n " in IR TZ star catalogue as criterion, by tetra-wave bands of WISE in IR TZ star catalogue (W1, W2, W3,
W4) magnitude is converted into based on the flow F waiting luminosity frequency v (iso)v(iso)。
Any value during a) " if color_n " meets " 1 color_n 4 ", then calculate front 3 wave bands with formula (1)
(i.e. W1, W2, W3) flow, and with formula (2) calculate the 4th wave band (i.e. W4) flow:
Wherein FvwxFor certain star WISE Wx (x=1,2,3,4) wave band wait luminosity flow with frequency representation, single
Position Jy；Fvwx(iso) be Wx wave band Vega with frequency representation wait luminosity flow, unit Jy, corresponding to " the F in table 2.v*
(iso) " item；fcwxFor Wx (x=1,2,3,4) this star of wave band with the correction factor of the flow zero point of frequency representation, dimensionless is right
" f_c (Wx) " item in Ying Yubiao 1. (x=1,2,3,4, as x=1, it is the item of " f_c (W1) ")；M (wx) is that this star exists
The Wx wave band magnitude of WISE.
B) other situations, then four wave bands are all with formula (1) calculated flow rate.
Deng luminosity method of flow introduce: with WISE system keep consistent, employing based on etc. luminosity wavelength (isophotal
Wavelengths, λ (iso)) and etc. luminosity flow (isophotal flux Fλ(iso)) spectrum reconstruction method (Tokunaga
Et al.2005), determine that Vega is respectively 3.3526,4.6028 in the luminosity wavelength X (iso) that waits of tetra-wave bands of WISE,
11.5608, and 22.0883 μm (Wright et al.2010), the flow at these four wavelength corresponding is Vega at this ripple
The meansigma methods of the intrinsic flow of section, referred to as waits luminosity flow Fλ(iso).WISE is defined in its four wave bands, wait luminosity flow with
The flow that luminosity flow is identical that waits of Vega is each wave band flow zero point (being shown in Table 2), and this flow zero point (magnitude zero point) defines
Method is equally applied to carry out U.S.'s Spitzer space telescope of IR wave band observation and Japan's AKARI space telescope.For
The star that spectral type is different from Vega, its spectral power distribution (SED) and Vega also has a difference, therefore, to from different spectral types
Star, its each wave band flow zero point also can make respective color correction.
Table 2.WISE magnitude null characteristic
Step 4: determine and expand the flow fitting function of every star in star catalogue
With the value of " color_n " in IR TZ star catalogue as criterion, determine the flow matching letter of each star in IR TZ star catalogue
Number.And determine the coefficient of correspondence of functional equation.The value of " color_n " is integer.We are according to the value of color_n, divide three kinds
Situation processes:
(1) when color_n is the integer meeting 3≤color_n≤4 conditions, this star streaming amount and frequency with one three times
Spline-Fitting.
Utilize WISE front 3 wave bands (W1, W2, W3, W4) waits luminosity frequency v (iso) (seeing table 2.) and every star
Flow at this wave band determines fitting parameter；Then, with a certain expansion wave band (W of IR-TZ star catalogueTZ1) wait luminosity frequency vTZ1
(iso) as input quantity, program output is this wave band flow value Fv of IR-TZ star catalogueTZ1, unit Jy.
(2) when color_n is the integer meeting 100≤color_n≤1131 condition, the fitting function of this star streaming amount is
Formula (3).
Fv is flow, unit Jy, obtains from step 3 calculates；V be each wave band of WISE etc. luminance frequency, unit
In the value of Jy, v the 7th row " v (iso) " from table 2., correspondence is chosen；A and b is constant coefficient, and the value of a is equal to " color_n "
Value, b by input front 3 the wave band v (iso) of WISE and flow Fv try to achieve.
(3) when color_n is " NULL ", illustrated that corresponding wave band magnitude data is abnormal, this star streaming amount wouldn't have been appointed
Where is managed.
Step 5: according to the continuous spectrum fitting function of Vega high accuracy spectrum, determines that zero star such as grade is opened up in expanding star catalogue
That opens up wave band waits luminosity wavelength XTZ1(iso) luminosity frequency v, is waitedTZ1(iso), and correspondence this wave band with wavelength represent etc.
Luminosity flow FλTZ1(iso), and with frequency representation etc. luminosity flow Fv TZ1(iso)
(1) because understanding that each wave band relative spectrum of IR TZ scope responds (RSR) situation, temporarily with each wave band RSR=
1 calculates, and therefore takes centre wavelength for waiting luminosity wavelength XTZ1(iso)。
(2) obtain some and expand wave band (WTZ1) λTZ1(iso) the luminosity flow F such as this corresponding wave bandλTZ1(iso)。
Utilize the formula (2) in Wright et al.2010, it is thus achieved that formula (4), and based on formula (4). try to achieve correspondence etc.
The luminosity flow F such as Vega monochromatic flux at luminosity wavelength, i.e. this wave bandλ(iso)。
λ unit is μm, FλUnit is W m‐2μm‐1, it is adaptable to 2.5 < λ < 29 μm
According to vFV=λ FλFormula (5)
Obtain this expansion wave band (WTZ1) with frequency representation wait luminosity flow FvTZ1(iso)
Respectively following (in " [] "): the F of amount unitv(iso) [Jy], λ (iso) [μm], c=2.99792458 × 1014μm
s‐1,Fλ(iso)[W cm-2μm‐1]
(3) according to vFv=λ FλObtain this expansion wave band (WTZ1) wait luminosity frequency vTZ1(iso)。
Respectively amount unit following (in " [] "): v (iso) [Hz], Fv(iso)[Jy],λ(iso)[μm],Fλ(iso)[W
cm-2μm‐1]
Step 6: in acquisition expansion star catalogue, each target source is at the flow value F expanding wave bandv TZ1(iso)source
Luminosity frequency (the v such as the IR TZ star catalogue a certain expansion wave band that step 5 is obtainedTZ1(iso) plan of step 4) is substituted into
Close function and the formula (4) of formula (3) and step 5, obtain in IR TZ star catalogue each star at the flow value F of this expansion wave bandv TZ1
(iso)source(in units of Jy).
Step 7: with Vega at the flow of this wave band for flow zero point (i.e. magnitude zero point), it is thus achieved that expand in star catalogue each
Target source is expanding the magnitude of wave band
In the IR TZ star catalogue obtain step 6, each star expands wave band (W at someTZ1) flow value Fv TZ1
(iso)sourceZero star such as grade obtained with step 5 substitutes into formula (8) at the luminosity flow that waits of this expansion wave band, it is thus achieved that IR TZ star
In table, each star is at a certain expansion wave band (WTZ1) the magnitude being flow zero point (i.e. magnitude zero point) with the flow of Vega, and use
Similar method obtains expands other expansion wave band magnitudes of star catalogue, completes IR TZ star catalogue.
Wherein, FV(iso)sourceFor the luminosity flow value such as grade of the target source of described expansion wave band, FV(iso)0Open up for described
The luminosity flow value such as grade of zero star such as grade (i.e. Vega) of exhibition wave band.
This expanding method is utilized to expand wavelength to 3.6um, 4.5um, 5.8um, 8.0um based on the infrared star catalogue of WISE
Four wave bands obtain expand star catalogue.It is respectively 0.070 with Spitzer satellite (another infrared satellite) official Catalog comparison error
Magnitude, 0.158 magnitude, 0.226 magnitude and 0.249 magnitude (wherein further comprises two satellites System level gray correlation each other), demonstrate
This expanding method is believable.
Claims (9)
1. infrared band flow based on infrared star catalogue expands computational methods, and existing known infrared star catalogue is made by described method
For fundamental catalog, by waiting luminosity wavelength and waiting luminosity method of flow and classification approximating method to realize the expansion of infrared band, raw
Becoming the star catalogue of infrared any wave band, the star catalogue of described infrared any wave band is for expanding star catalogue, it is characterised in that described method includes
Following steps:
Step one: selection known infrared star catalogue, screens satisfactory target source, extracts relevant parameter item；
Step 2: calculate the infrared colour index of all target sources in described expansion star catalogue, and accurately divide based on parameters such as colour indexs
Class；
Step 3: based on wait luminosity wavelength and wait luminosity method of flow by expand the magnitude of four wave bands in star catalogue be converted into based on
Flow Deng luminosity frequency；
Step 4: determine the flow fitting function of every star in described expansion star catalogue；
Step 5: according to the continuous spectrum fitting function of Vega high accuracy spectrum, determines that Vega expands ripple in expanding star catalogue
Section wait luminosity wavelength, etc. luminosity frequency and correspondence thereof this wave band respectively with wavelength and frequency representation etc. luminosity flow；
Step 6: in acquisition expansion star catalogue, each target source is at the flow value expanding wave band；
Step 7: with Vega at the flow of this wave band for flow zero point, it is thus achieved that in described expansion star catalogue, each target source is being expanded
The magnitude of wave band.
2. method as claimed in claim 1, it is characterised in that described step one specifically includes:
(1) based on required expansion wave band and the sky distribution situation of target source, investigate and select applicable known infrared star catalogue, use
Make the fundamental catalog expanded；
(2) fundamental catalog coordinate and each infrared band magnitude are screened, select required four wave bands at least 3 in fundamental catalog
The target source of individual wave band effectively observation, is formed and expands star catalogue；
(3) extract and expand coordinate and the known infrared magnitude important parameter item of each four wave bands of target source in star catalogue, described four
Wave band represents with W1, W2, W3 and W4 successively from being short to length.
3. method as claimed in claim 1, it is characterised in that described step 2 specifically includes:
(1) infrared colour index W1-W2 of all target sources, W2-W3 and W3-W4 in expansion star catalogue is calculated；
(2) to expand W2-W3 colour index in star catalogue as main criterion, W2-W3 colour index is as secondary criterion, to expanding in star catalogue
All target classifications, are divided into 16 subclasses；
(3) to meet main criterion with time criterion as condition simultaneously, four wave band flow zero points described in each target are selected to repair accordingly
Positive coefficient fc, carries out flow zero point correction by affiliated subclass described four wave bands corresponding to each target；
(4) according to judged result, in expanding star catalogue, a columns is added, to record judged result, the named color_ of described row
n；Described color_n row numerical value be a, a be integer.
4. as claimed in claim 1 method, it is characterised in that described step 3 particularly as follows:
To expand in star catalogue, the numerical value of color_n row is as criterion, by four wave band W1 described in expansion star catalogue, W2, W3, W4 magnitude
It is converted into based on the flow waiting luminosity frequency；
If color_n meets 1 color_n 4, then W1, the formula of the luminosity flows such as W2, W3 calculating is:
The formula of the luminosity flows such as W4 calculating is:
If color_n is unsatisfactory for 1 color_n 4, then with calculating W1, the public affairs waiting luminosity flow of tetra-wave bands of W2, W3, W4
Formula is formula (1)
Wherein X=1,2,3,4；
For certain star fundamental catalog WX wave band with frequency representation wait luminosity flow, unit is Jy；
FV(iso)WXFor WX wave band Vega with frequency representation wait luminosity flow, unit Jy；
For this star of WX wave band with the correction factor of the flow zero point of frequency representation, dimensionless；
mWXFor this star at the WX wave band magnitude of fundamental catalog.
5. method as claimed in claim 1, it is characterised in that described step 4 specifically includes:
The value of color_n in expansion star catalogue, as criterion, determines and expands the flow fitting function of each star in star catalogue, and determine
The coefficient of correspondence of functional equation, the value of color_n is integer, and we are according to the value of color_n, and point three kinds of situations process
(1) when the integer that color_n is satisfied-3≤color_n≤4 condition, this star streaming amount and frequency are by a cubic spline
Function Fitting；Described cubic spline function refers to be the function of cubic polynomial in each minizone；
(2) when color_n is the integer meeting 100≤color_n≤1131 condition, the fitting function of this star streaming amount is:
FVFor flow, unit Jy, obtain from step 3 calculates；V be each wave band of WISE etc. luminance frequency, unit Jy；A and b
Being all constant coefficient, the value of a value equal to color_n, b is asked by input front 3 wave bands of WISE and flow in formula (3)
?；
(3) when color_n is " NULL ", illustrated that corresponding wave band magnitude data is abnormal, this star streaming amount wouldn't have been made any place
Reason.
6. method as described in claim 1-4 is arbitrary, it is characterised in that described step 5 specifically includes:
(1) because wouldn't clearly expand each wave band relative spectrum response RSR situation of scope, calculate with each wave band RSR=1 temporarily,
Therefore taking centre wavelength is to wait luminosity wavelength；
(2) luminosity flows such as expanding this wave band corresponding to wave band is obtained；
The luminosity flows such as Vega monochromatic flux at the luminosity wavelength such as correspondence, i.e. this wave band are tried to achieve based on formula 4.
vFV=λ FλFormula (5)
The described expansion wave band luminosity flow such as grade with frequency representation is obtained according to formula (5)
(3) the luminosity frequency such as grade of described expansion wave band is obtained according to formula (5)
FλFor luminosity flows such as wave bands；FV(iso) it is the wave band luminosity flow such as grade with frequency representation；ν (iso) is to wait luminosity frequency；
λ (iso) is to wait luminosity wavelength；ν (iso) unit Hz, FV(iso) unit Jy, λ (iso) unit μm, c=2.99792458 × 1014
μm s‐1,Fλ(iso) unit W cm-2μm‐1, it is adaptable to 2.5 < λ < 29 μm.
7. method as claimed in claim 6, it is characterised in that described step 6 specifically includes:
Step 5 obtained expands fitting function and the formula (3) expanding the luminosity frequency substitution step 4 such as wave band described in star catalogue
And the formula (4) of step 5, obtaining expanding in star catalogue that each star is at the flow value of described expansion wave band, described flow value is with Jy as list
Position.
8. method as claimed in claim 7, it is characterised in that described step 7 specifically includes:
The star such as zero that each star in star catalogue obtains at the flow value of described expansion wave band and step 5 of expanding step 6 obtained exists
The luminosity flow value that waits of described expansion wave band substitutes into
Wherein, FV(iso)sourceFor the luminosity flow value such as grade of the target source of described expansion wave band, FV(iso)0For described expansion ripple
The luminosity flow value such as grade of zero star such as grade of section.
Obtain and expand the magnitude that each star in star catalogue is flow zero point at the flow with Vega of a certain expansion wave band, and with being similar to
Method obtain expand star catalogue other expand wave band magnitudes, complete expand star catalogue.
9. method as claimed in claim 8, it is characterised in that described fundamental catalog is the release of U.S. WISE space telescope whole day
Source table.
Priority Applications (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN201610430215.6A CN106055700B (en) | 2016-06-16 | 2016-06-16 | A kind of infrared band flow expansion calculation method based on infrared star catalogue |
Applications Claiming Priority (1)
| Application Number | Priority Date | Filing Date | Title |
|---|---|---|---|
| CN201610430215.6A CN106055700B (en) | 2016-06-16 | 2016-06-16 | A kind of infrared band flow expansion calculation method based on infrared star catalogue |
Publications (2)
| Publication Number | Publication Date |
|---|---|
| CN106055700A true CN106055700A (en) | 2016-10-26 |
| CN106055700B CN106055700B (en) | 2019-07-19 |
Family
ID=57167586
Family Applications (1)
| Application Number | Title | Priority Date | Filing Date |
|---|---|---|---|
| CN201610430215.6A Active CN106055700B (en) | 2016-06-16 | 2016-06-16 | A kind of infrared band flow expansion calculation method based on infrared star catalogue |
Country Status (1)
| Country | Link |
|---|---|
| CN (1) | CN106055700B (en) |
Cited By (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN108279221A (en) * | 2017-12-07 | 2018-07-13 | 中国科学院国家天文台 | A kind of part day area atmospheric transparency acquisition methods |
| CN115015243A (en) * | 2022-04-18 | 2022-09-06 | 中国科学院云南天文台 | Method for determining fixed star physical parameters in batches based on photometric data |
Citations (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN102201008A (en) * | 2011-06-17 | 2011-09-28 | 中国科学院软件研究所 | GPU (graphics processing unit)-based quick star catalogue retrieving method |
| CN103884336A (en) * | 2014-03-20 | 2014-06-25 | 北京控制工程研究所 | Establishment method of daytime star sensor-based infrared star detection navigation star catalogue |
-
2016
- 2016-06-16 CN CN201610430215.6A patent/CN106055700B/en active Active
Patent Citations (2)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN102201008A (en) * | 2011-06-17 | 2011-09-28 | 中国科学院软件研究所 | GPU (graphics processing unit)-based quick star catalogue retrieving method |
| CN103884336A (en) * | 2014-03-20 | 2014-06-25 | 北京控制工程研究所 | Establishment method of daytime star sensor-based infrared star detection navigation star catalogue |
Non-Patent Citations (2)
| Title |
|---|
| T.H.JARRETT等: "The Spitzer-WISE Survey of The Ecliptic Poles", 《THE ASTROPHYSICAL JOURNAL》 * |
| 张磊等: "快速全天自主星图识别", 《光学精密工程》 * |
Cited By (3)
| Publication number | Priority date | Publication date | Assignee | Title |
|---|---|---|---|---|
| CN108279221A (en) * | 2017-12-07 | 2018-07-13 | 中国科学院国家天文台 | A kind of part day area atmospheric transparency acquisition methods |
| CN108279221B (en) * | 2017-12-07 | 2021-04-13 | 中国科学院国家天文台 | Method for acquiring atmospheric transparency of local sky area |
| CN115015243A (en) * | 2022-04-18 | 2022-09-06 | 中国科学院云南天文台 | Method for determining fixed star physical parameters in batches based on photometric data |
Also Published As
| Publication number | Publication date |
|---|---|
| CN106055700B (en) | 2019-07-19 |
Similar Documents
| Publication | Publication Date | Title |
|---|---|---|
| Calvi et al. | Bright galaxies at Hubble’s REDSHIFT detection frontier: Preliminary results and design from the redshift z∼ 9–10 BoRG pure-parallel HST survey | |
| Gavazzi et al. | RINGFINDER: automated detection of galaxy-scale gravitational lenses in ground-based multi-filter imaging data | |
| Petit et al. | PolarBase: a database of high-resolution spectropolarimetric stellar observations | |
| Popescu et al. | Near-infrared colors of minor planets recovered from VISTA-VHS survey (MOVIS) | |
| Coil et al. | The prism multi-object survey (PRIMUS). I. Survey overview and characteristics | |
| Rodney et al. | SN Refsdal: photometry and time delay measurements of the first Einstein cross supernova | |
| Maguire et al. | Hubble Space Telescope studies of low-redshift Type Ia supernovae: evolution with redshift and ultraviolet spectral trends | |
| Popescu et al. | Taxonomic classification of asteroids based on MOVIS near-infrared colors | |
| Timlin et al. | SpIES: The Spitzer IRAC Equatorial Survey | |
| Hung et al. | Sifting for sapphires: systematic selection of tidal disruption events in iPTF | |
| Schmidt et al. | The largest M Dwarf flares from ASAS-SN | |
| Udalski et al. | The Optical Gravitational Lensing Experiment. OGLE-III Photometric Maps of the Small Magellanic Cloud | |
| Dunham et al. | Young stellar objects in the Gould Belt | |
| Bayliss et al. | SPT-GMOS: a Gemini/GMOS-South spectroscopic survey of galaxy clusters in the SPT-SZ survey | |
| Nord et al. | Observation and confirmation of six strong-lensing systems in the Dark Energy Survey science verification data | |
| Gao et al. | Random forest algorithm for classification of multiwavelength data | |
| Brunker et al. | Properties of the KISS Green Pea Galaxies | |
| Ko et al. | To the Edge of M87 and Beyond: Spectroscopy of Intracluster Globular Clusters and Ultracompact Dwarfs in the Virgo Cluster | |
| Allen et al. | A new brown dwarf desert? A scarcity of wide ultracool binaries | |
| Kim et al. | The Infrared Medium-deep Survey. VI. Discovery of Faint Quasars at z∼ 5 with a Medium-band-based Approach | |
| Hubrig et al. | Rotationally modulated variations and the mean longitudinal magnetic field of the Herbig Ae star HD 101412 | |
| CN106055700A (en) | Infrared band flux expansion calculation method based on infrared star catalogue | |
| Golden-Marx et al. | The high-redshift Clusters Occupied by Bent Radio AGN (COBRA) survey: follow-up optical imaging | |
| Hsu et al. | Near-infrared Survey and Photometric Redshifts in the Extended GOODS-North Field | |
| Lee et al. | Properties of M31. IV. Candidate luminous blue variables from PAndromeda |
Legal Events
| Date | Code | Title | Description |
|---|---|---|---|
| C06 | Publication | ||
| PB01 | Publication | ||
| C10 | Entry into substantive examination | ||
| SE01 | Entry into force of request for substantive examination | ||
| GR01 | Patent grant | ||
| GR01 | Patent grant |