Tutorial 9: Photometric colour calibration¶

Goal: set the colour balance of the picture from the stars in it, so that a star the colour of the Sun is neutral and the sky is a neutral grey. You finish with calibrated.fits, a table of the stars used (stars.csv) and a stretched picture with the cast gone.

Data: solved.fits, the plate-solved IC 5070 image from tutorial 8: linear, colour, with a world coordinate system. It also needs the Gaia catalogue, because it takes the colours of catalogue stars from it (the BP-RP colour, which is the difference between Gaia's blue and red magnitudes: about 0.8 for the Sun, 0.3 for a hot blue star, 2 for a cool red one).

What happens. The solved positions are used to find Gaia stars in the image; each star is measured through the same aperture in red, green and blue; a line of instrumental colour against true colour is fitted for red against green and for blue against green; and the gains that make a star of BP-RP 0.82 (like the Sun) neutral are found. Then the sky of the three planes is brought to one level. The method is in How colour calibration works.

When. On a linear image, after background extraction and plate solving, before stretching.

Step 1: Calibrate¶

valerian photocal solved.fits -o calibrated.fits --stars-out stars.csv

36 Gaia stars measured, 33 used; aperture radius 5.1 px; neutral at BP-RP 0.82
  red against green: slope -0.635 mag per BP-RP, scatter 0.027 mag, gain 0.7547 +/- 0.0032
 blue against green: slope +0.080 mag per BP-RP, scatter 0.024 mag, gain 0.9860 +/- 0.0037
sky before 610.76 597.29 608.32, after 552.68 552.68 552.68 (offsets -91.76 44.61 47.15)
wrote the star table stars.csv
wrote calibrated.fits

The command took 0.34 s. Reading it:

• 36 Gaia stars measured, 33 used; aperture radius 5.1 px. 36 catalogue stars in the field were bright enough to measure (Gaia G between 6 and 11, with enough signal in every colour) and 33 were kept after rejecting outliers. The measuring aperture is 2 times the median FWHM of the stars (2.56 pixels). At least 15 stars are needed (--min-stars).
• neutral at BP-RP 0.82. The colour made neutral: a G2 dwarf like the Sun, --reference-colour.
• red against green: slope -0.635 mag per BP-RP, scatter 0.027 mag, gain 0.7547 +/- 0.0032. For each star the instrumental red-minus-green magnitude is plotted against its true BP-RP. The points lie on a line with a slope of -0.635 mag per unit of BP-RP, within 0.027 mag. The gain is the factor that puts a BP-RP 0.82 star on zero: the red plane is multiplied by 0.7547. Its uncertainty is 0.0032, 0.4 per cent.
• blue against green: ... gain 0.9860 +/- 0.0037. The same for blue: the blue plane is multiplied by 0.9860. Green is the reference and stays at 1, so the brightness is kept.
• sky before 610.76 597.29 608.32, after 552.68 552.68 552.68 (offsets -91.76 44.61 47.15). After the gains, a constant is added to each plane so the sky has one level (552.68) in all three, which makes the background a neutral grey. The offsets are the constants (red is pulled down by 91.76 ADU, green and blue lifted by 44.61 and 47.15).

calibrated.fits has the gains and the offsets in its header: PCCGAINR 0.7547, PCCGAING 1.0, PCCGAINB 0.9860, PCCOFFR -91.76, PCCOFFG 44.61 and PCCOFFB 47.15. stars.csv has one line per star measured: its pixel position (x, y), Gaia magnitude g and colour bp_rp, the fluxes in red, green and blue and used (1 if it went into the fit). Here it has 36 stars, 33 used, with g from 7.0 to 11.0 and bp_rp from 0.35 to 2.15, a good spread of colours, which is what makes the fit reliable.

x,y,g,bp_rp,flux_r,flux_g,flux_b,used
206.029,1586.533,7.000,1.000,571262.861,367588.606,382001.901,1
956.491,1635.028,8.000,2.125,209667.817,76182.253,67570.169,1

The stars it measured, over a screen-stretched picture of the same image: green circles are the 33 used, red circles the 3 that were rejected as outliers.

Step 2: See the difference¶

The sky and the stars are the proof. Left: flat.fits stretched (stretched.fits, tutorial 6), which has the cast of the data: the sky is a dark purple. Right: calibrated.fits with the same automatic stretch (valerian stretch calibrated.fits -o cstretched.fits). Both are Valerian's stretched output at one third of the size.

valerian stretch calibrated.fits -o cstretched.fits --preview cstretched.png

black 532.4390, white 5099.4653, Mtf { midtone: 0.0385596760748138 }
plane 0: median 552.7506 -> 0.1002
plane 1: median 552.7175 -> 0.1001
plane 2: median 552.7233 -> 0.1001
wrote cstretched.fits
wrote preview cstretched.png

Now the three planes' sky medians land on 0.1002, 0.1001 and 0.1001: the sky is neutral grey. Before the calibration they were 0.1209, 0.0663 and 0.1113, tutorial 6's log. The sky has lost its tint. The nebula looks fainter, because the red gain of 0.75 turns the red down: a harder stretch brings it back.

valerian info calibrated.fits --stats gives the sky of every plane as 552.7. The image, linear, ready to stretch to taste or to remove the stars from (tutorial 7 on calibrated.fits works the same way).

Options used¶

All options are in the command line reference.

What the options changed on this image (the gains are red and blue; the sky is "after"):

Red and blue gains for each option on the same image, from the table above: the reference colour moves the red gain most.

Stars measured and stars used in the fit for each option, from the table above.

The gains are stable: dropping the fainter stars (--max-mag 10, half the stars), the brightest (--min-mag 8), changing the aperture or restricting the colour range moves the gains by less than 0.02. That stability, not the size of the scatter, is what tells you the calibration is sound. A different --reference-colour shifts the whole balance: a redder reference (1.2) lowers the red gain to 0.60, because the stars it makes neutral are red. --min-snr 30 changed nothing: every star already had a signal-to-noise above 30. --no-neutralise applies the gains but not the offsets: the planes' skies stay at their own levels (red 460.92, green 597.29, blue 599.83), and the sky is not grey.

How to tell it worked¶

• N Gaia stars measured, M used with M at least 15 (here 33).
• scatter is a few hundredths of a magnitude (0.027 and 0.024), and the gain's +/- is under 1 per cent.
• The gains are not extreme (here 0.75 and 0.99). As a rule of thumb, a gain far from 1, say below 0.5 or above 2, deserves a look at stars.csv.
• The after sky is one number in all planes.
• stars.csv has stars of different colours (here BP-RP 0.35 to 2.15) and mostly used 1.
• The stretched picture has a neutral dark sky.
• Changing the options a little (magnitude limits, aperture) leaves the gains within 2 per cent.

Troubleshooting¶

valerian: this image has been stretched; colour calibration works on the linear image. You gave a stretched file (here stretched.fits). Run photocal on the linear one, after the background extraction and before the stretch.

valerian: master_dark.fits has no world coordinate system and the header lacks a position and scale to solve one: runvalerian solvefirst. The image has no WCS and no RA, DEC and scale to solve one from (here a mono master dark, which is not a colour image anyway). Plate solve first (tutorial 8), or give the solution with --wcs. If the header has a position and scale photocal solves for itself: valerian photocal flat.fits printed no WCS in the image: solving it from the header first and gave the same result.

valerian: colour calibration needs at least 40 usable stars and found 36 of 36 measured: the field is sparse for the catalogue, or the stars are too faint for --min-snr .... --min-stars 40 was given and the field has 36 stars the catalogue can offer. Fewer stars means a less certain fit. A field narrower than about half a degree has too few stars brighter than G = 11: use a deeper catalogue (see tutorial 8), or lower --min-stars if you accept a less certain gain (the +/- tells you how much).

The scatter is large (0.1 mag or more) or the gains have large +/-. The stars are measured badly: saturated bright stars (raise --min-mag), faint noisy ones (raise --min-snr, lower --max-mag), or crowded ones in a nebula (a smaller --aperture). The used column of stars.csv and the red circles in the picture show which stars were rejected.

The sky is still tinted, or the nebula has lost its colour. photocal balances the sky and the stars; the nebula's colour is whatever is left. If the sky has gradients in colour, run background extraction first (it is per plane); if the data was stretched before, it cannot be fixed.

The result looks too blue or too red. The reference is the Sun, BP-RP 0.82. For a different taste, change --reference-colour (0.5 gave red and blue gains of 0.91 and 0.96, 1.2 gave 0.60 and 1.01).

The input has one plane. photocal needs red, green and blue planes; a mono image has no colour to calibrate.

The desktop app¶

In the desktop app this is the Colour tool of step 4, Process: see the reference.

Where next¶

calibrated.fits is the finished linear colour image. Stretch it to taste (tutorial 6), or take the stars out (tutorial 7). Tutorial 10 shows how to get more resolution from the same frames.