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Space-­Based   Galaxy   Survey   Exposure   Time   Calculator   

Version   10   

User   Manual   &   Code   Description

   

   

Point   of   Contact:   

Christopher   M.   Hirata   

Caltech   M/C   350-­17,   Pasadena,   CA   91125,   USA

   

chirata@tapir.caltech.edu   

March   28,   2012   

   

Table   of   Contents   

   

1.

   

OVERVIEW......................................................................................................................................................2

   

2.

   

COMPILING   THE   CODE ...............................................................................................................................3

   

A.

   

A

DDITIONAL FLAGS

.......................................................... 3

   

3.

   

RUNNING   THE   CODE ...................................................................................................................................5

   

A.

   

S

PECIFYING THE TELESCOPE CONFIGURATION

........................................ 5

   

B.

   

T

ELESCOPE CONFIGURATION FILE FORMAT

.......................................... 7

   

C.

   

S

PECIFYING THE OBSERVING STRATEGY AND DETECTOR CHARACTERISTICS

..................... 8

   

D.

   

WL-

SPECIFIC INPUTS

....................................................... 10

   

E.

   

BAO-

SPECIFIC INPUTS

...................................................... 12

   

F.

   

PZCAL-

SPECIFIC INPUTS

.................................................... 15

   

4.

   

CODE   OUTPUTS:   WL   ETC ........................................................................................................................ 15

   

5.

   

CODE   OUTPUTS:   BAO   ETC ...................................................................................................................... 17

   

6.

   

CODE   OUTPUTS:   PZCAL   ETC.................................................................................................................. 18

   

7.

   

DETAILED   METHODOLOGY   AND   ASSUMPTIONS............................................................................ 19

   

A.

   

B

ACKGROUND COSMOLOGY

..................................................... 19

   

B.

   

S

KY BRIGHTNESS

.......................................................... 19

   

C.

   

G

ALACTIC EXTINCTION

...................................................... 20

   

D.

   

L

INE SENSITIVITY AND EFFECTIVE SOLID ANGLE

.................................... 20

   

E.

   

E

XPECTED VS

.

 OBSERVED 

SNR................................................. 22

   

F.

   

N

OISE MODEL

............................................................. 24

   

G.

   

T

HERMAL BACKGROUND MODEL

.................................................. 27

   

H.

   

G

ALAXY PROFILES

......................................................... 29

   

I.

   

P

OINT SPREAD FUNCTIONS

.................................................... 29

   

J.

   

E

LLIPTICITY UNCERTAINTY

................................................... 32

   

8.

   

DATA   STRUCTURES   AND   FUNCTIONS ................................................................................................ 33

   

A.

   

D

ATA STRUCTURES

......................................................... 33

   

B.

   

I

NTERFACE FUNCTIONS

...................................................... 34

   

C.

   

S

PECIAL FUNCTIONS

........................................................ 34

   

D.

   

R

OUTINES TO SET UP DETECTOR PARAMETERS

....................................... 35

   

E.

   

R

OUTINES TO COMPUTE THE THROUGHPUT

.......................................... 35

   

Summary of Contents for Spice-Based Galaxy Calculator

Page 1: ...D WL SPECIFIC INPUTS 10 E BAO SPECIFIC INPUTS 12 F PZCAL SPECIFIC INPUTS 15 4 CODE OUTPUTS WL ETC 15 5 CODE OUTPUTS BAO ETC 17 6 CODE OUTPUTS PZCAL ETC 18 7 DETAILED METHODOLOGY AND ASSUMPTIONS 19 A B...

Page 2: ...s The ETC is written in standard C and does not link to any external libraries This should make it easier for users to install and run as well as avoiding legal issues with copyrighted code The ETC al...

Page 3: ...prefer to cover sky at as fast a rate as possible while maintaining high data quality redundancy and low overheads or are constrained to the survey rate of another program 2 Compiling the Code The ET...

Page 4: ...0 thereby enabling opposite dispersion direction for configurations with a single spectrometer These two options should not be used together in v7 and later an error message is generated Options to as...

Page 5: ...window closes when the program exits Options no longer supported The DCCD_MODE option no longer exists removed in v9 since the detector type is specified at runtime 3 Running the Code Both the WL and...

Page 6: ...ve f1 fall but see the note below on scattered light A from file input might look like baoetc exe Enter telescope configuration 0 generic 1 from file 1 Input file name data JDEM_Omega_nomask_SpC dat U...

Page 7: ...cters An explicit example of a configuration file is data JDEM_Omega_nomask_SpC dat which has the form1 JDEM Omega no pupil mask based on Throughput table JDEM Omega 110322_cj xlsx Received 2011 03 23...

Page 8: ...5076 0 5103 0 5562 0 5426 2 0000 0 7109 0 6934 The THERMAL line like all lines in the configuration file is limited to no more than 254 characters The 7 parameters specified are in order The telescop...

Page 9: ...ntend for no additional filter losses to be considered The read noise floor is in effective electrons rms per exposure For CCDs this is the entire read noise for NIR detectors this is added in quadrat...

Page 10: ...alaxies a cut e max on the ellipticity error e of galaxies to be measured and the galaxy catalog to use to estimate source densities Example inputs are Enter minimum resolution factor 0 4 Enter maximu...

Page 11: ...07 25 34 24 27 23 39 The file begins with a set of comment lines starting with comment lines must be at the beginning and not interspersed through the file The first non comment line has three entries...

Page 12: ...he conditional size probability distribution P reff LH z The code is currently configured to take a population model that is a non negative integer of the form 10i j where i indicates the choice of H...

Page 13: ...searches 15 The Schechter function parameters have had the following corrections applied i correction to the WMAP 5 year cosmology Sobral et al used H0 70 km s 1 Mpc 1 and m 0 3 ii conversion back to...

Page 14: ...selected and split into bins based on the H flux FH W m 2 For five bins in log10 FH W m 2 centered at 19 0 0 2 18 2 and in two wavelength ranges 1 1 1 5 and 1 5 2 0 m the effective radii are well fit...

Page 15: ...0000E 03 e pix s Noise variance per unit solid angle in one exposure sky only 1 68592E 03 e 2 arcsec 2 total 3 90252E 03 e 2 arcsec 2 Source counts per exposure at AB mag 20 2 11038E 04 e at AB mag 21...

Page 16: ...3 4175 3 0460 0 69454 23 39012 18 000 0 50119 4 0062 2 8030 0 74110 23 30384 18 000 0 56234 4 7299 2 6021 0 78278 23 21368 18 000 0 63096 5 6214 2 4354 0 81939 23 11995 18 000 0 70795 6 7216 2 2967 0...

Page 17: ...E 03 Weak lensing n 6 59516E 04 gal deg 2 1 83199E 01 gal arcmin 2 Weak lensing n_eff 6 05045E 04 gal deg 2 1 68068E 01 gal arcmin 2 5 Code Outputs BAO ETC The BAO ETC returns a table of galaxy yields...

Page 18: ...in the FH reff plane The code also returns summary statistics Summary statistics Sky background flux 3 08083E 00 e pix s Thermal background flux 1 38794E 01 e pix s telescope 8 75479E 02 e pix s upstr...

Page 19: ...yields which are not computed in PZCAL mode 7 Detailed Methodology and Assumptions A Background cosmology The background cosmology assumed for number density yields in the BAO mode is the same as tha...

Page 20: ...bjects in the imager follow an analogous procedure with the exceptions that i the 1st order throughput f1 is replaced with the 0th order throughput f0 ii one uses a polychromatic rather than monochrom...

Page 21: ...f 0 G 0 0 1 Also we can see that for a top hat distribution where the probability density is equal to 1 within some region of angle and 0 elsewhere the effective area is eff hence its name Smaller sol...

Page 22: ...SNRe for optimal extraction and SNRo can be obtained from elementary statistics We consider an image of size n pixels to form a data vector d Rn and define an inner product of two vectors d and e bas...

Page 23: ...f galaxies e g H emitters at a given redshift there is some probability distribution per Mpc3 SNRe and correspondingly a cumulative distribution SNRe x dx SNRe We need to know the number density of ga...

Page 24: ...order Z 2 the number density of objects with SNRo Z can be computed as the arithmetic average of the number with SNRe greater than Z 1 1 2 Z 1 and greater than Z 1 1 2 Z 1 This provides a simple appr...

Page 25: ...t behavior can be changed by several options The DLOGICAL_READ_FLOOR option takes only the larger of the two read noise related terms in eff 2 If a CCD detector is specified the ETC simply adds the Po...

Page 26: ...same impact on the SNR The second integral in terms of the Fourier transform is actually implemented in the code For a Gaussian we would have J 0 33 EE50 but the code does the full integral whose val...

Page 27: ...tel and one neglected emission from all optics downstream of the secondary then there would be a consequent flux of detected photons per pixel per second per steradian given by dI d TfilterFbb Ttel 2...

Page 28: ...this emission fills the full solid angle admitted by any mask at the exit pupil The aft optics contribution is then Iaft 2 4 f 2 aftTfilter 1 aft 1 2 Fbb Taft 2 for the case without a pupil mask with...

Page 29: ...us using elementary geometry The MTF is further modified by jitter and charge diffusion These may in general have complicated forms but for the purposes of the ETC they are modeled by a Gaussian of wi...

Page 30: ...ing conservative in terms of evaluating the u integrals even in this case Between 0 125 and 0 175 we linearly interpolate between the two formulae An alternative model which can be specified by the DW...

Page 31: ...are typical values for WFIRST and for an emission line galaxy respectively The behavior of this correction is not a perfect representation since real line profiles are non Gaussian they vary across th...

Page 32: ...5 75 50 50 and 75 25 mixtures of defocus with the other three aberrations J Ellipticity uncertainty The uncertainty in the ellipticity is estimated by standard techniques 38 The result is that rather...

Page 33: ...e are three data structures currently in use one to describe a PSF one to describe throughput curves and one to describe telescope thermal parameters typedef struct double pixscale pixel scale in arcs...

Page 34: ...ft_net_emissivity Net emissivity of aft optics total of all surfaces in series double post_filter_rate Count rate in e pix s from structures downstream of the filter THERMAL_DATA This structure contai...

Page 35: ...ng detector effects at spatial frequency u v in cycles arcsec and using the PSF configuration in structure psf If psf is monochromatic this function acts as a wrapper to get_MTF_mono If psf is polychr...

Page 36: ...PSF_DATA psf double var_1exp double calib_1exp Returns the 1 uncertainty in the line flux in W m 2 from a galaxy for a single exposure as a function of reff in arcsec assumes exponential profile the...

Page 37: ...FHa int model void print_HaLF_model FILE fp int model The function get_HaLF obtains the H LF at redshift z and flux FH in W m 2 and using the specified galaxy model The result is in galaxies per comov...

Page 38: ...NeffdA char OutFile char outmode double get_dNdA_WL_gal double reffmin double reffmax double zmin double zmax char GalaxyCat double lambda_min double lambda_max PSF_DATA psf int N_exp double var_1exp...

Page 39: ...l background rate in electrons per pixel per second from the telescope primary and secondary mirrors and associated black surfaces at the same temperature spiders obscurations and baffles and radiatio...

Page 40: ...nd aft optics contributions the downstream components contribution is assumed to carry its own margin double getNoiseTotal double t_exp double ct double rnfloor int mode This routine computes the nois...

Page 41: ...only including a single H LF model and constant throughput Version 2 March 21 2011 Added support for telescope configuration files including separate all order and 1st order throughputs Version 3 Marc...

Page 42: ...ector options from macros to global variables set at the beginning of the run allows user to choose detector without recompiling Added DWFE_HOPKINS_EXP flag for alternative wavefront distribution Adde...

Page 43: ...ark Energy Mission JDEM Joint Dark Energy Mission configuration MDLF Minimum Detectable Line Flux MTF Modulation Transfer Function NIR Near InfraRed PSF Point Spread Function PZCAL Photometric Z redsh...

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