Evaluation of 6dF Data

Evaluation of 6dF Data

Lesa MooreMacquarie UniversityHonours Project 2003Supervisor: Quentin Parker MU/AAO

2

Goals of Honours Project

Independent evaluation of results from 6dFDR and RUNZ

Comparison analysis using IRAF dofibers, line measurements, xcsao and emsao

Test 6dFDR and RUNZ for accuracy and systematic errors by comparison with IRAF results

Test 6dFDR and RUNZ for repeatability Report to survey team with results and

recommendations

3

Target and Observed Fields One field studied to date

My first field!!

4

Field Details

0924m30 Observed 20/3/2002 Reflection gratings

600V: 4000-5600Å; 316R: 5500-8500Å 109 spectra, 28 parked fibres, 13 skies

5

Batch-Mode Reduction 6dFDR, RUNZ on separate V, R and

spliced VR data using 6dFDR arc-line lists (see later!)

IRAF dofibers on V, R data using my own arc-line lists (NIST Atomic Spectra Database: http://physics.nist.gov/cgi-bin/AtData/lines_form)

IRAF xcsao on R grating data only

No heliocentric correction applied (raw redshifts only)

6

Comparison Spectra - 1

IRAF data not flux-calibrated

7

Comparison Spectra - 2

IRAF data not flux-calibrated

8

Signal-to-noise comparison(mean for 109 galaxies)

RUNZ R 10.3500

RUNZ V 9.4253

RUNZ VR 8.8476

IRAF R 3.4753

Data from: IRAF - measured in splot; RUNZ - 0924Rcom.sdfz.zlog

9

Problems encountered

Discovered HgCdNe line list has too few Ne, extra Ar and miscellaneous lines

High-dispersion data: only 13 good arc lines in HgCdHe line list: - 6dFDR throws away 3 worst lines - can’t afford this!

Heliocentric correction incorrectly applied, correct on: /net/aaowfi/data1/will/runz/runz6df_may03

10

Arc spectrum R - HgCdNe

11

R-arc line-identification compared (subset of 10 fibres)

IRAF 6dFDR

# lines in line list

61 46

mean rms

of disp function

0.1930 0.1584

mean # lines fitted

39.5 29.5

Data from: IRAF – arcapid.t.ms; 6dFDR – arclist006.dat

On 108 spectra, mean rms IRAF 0.1816; 6dFDR 0.1539

12

Red reflection Full list My list for run5 RUNZ 1 2 3 4 7 8 10 11 12 13 1 2 3 4 7 8 10 11 12 135656.566 5656.566 1 1 15689.816 5689.816 1 1 15719.225 5719.225 1 1 1

20 Hg 5769.598 5769.598 5769.598 1 1 1 1 1 1 1 1 1 110 Hg 5790.663 5790.663 5790.663 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(500) Ne 5804.45 5804.4496(500) Ne 5820.156 5820.1558 1 1100 Ne 5852.488 5852.488 5852.488 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 120 Ne 5881.895 5881.895 5881.895 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 130 Ne 5944.834 5944.834 5944.834 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 110 Ne 5975.534 5975.534 5975.534 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 115 Ne 6029.997 6029.997 6029.997 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 130 Ne 6074.337 6074.337 6074.337 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 140 Ne 6096.163 6096.163 6096.163 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(300) Cd 6099.142(100) Cd 6111.49(100) Ne 6128.45 6128.4580 Ne 6143.062 6143.062 6143.062 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 120 Ne 6163.594 6163.594 6163.594 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 120 Ne 6217.281 6217.281 6217.281 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 140 Ne 6266.495 6266.495 6266.495 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 120 Ne 6304.789 6304.789 6304.789 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(100) Cd 6325.166(30) Cd 6330.01350 Ne 6334.428 6334.428 6334.428 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(1000) Ne 6382.991 6382.991 1 1 1 1 1 1 1 1 1 1100 Ne 6402.246 6402.246 6402.246 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 120 (2000)Cd 6438.47 6438.47 6438.47 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1100 Ne 6506.528 6506.528 6506.528 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 130 Ne 6532.882 6532.882 6532.882 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 130 Ne 6598.953 6598.953 6598.953 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(150) Ne 6652.092 6652.092 1 1 1 160 Ne 6678.276 6678.276 6678.276 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 135 Ne 6717.043 6717.043 6717.043 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(30) Cd 6778.11680 Ne 6929.467 6929.467 6929.467 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 11 Ar 6965.43 6965.43 6965.43 1 1 1 1 1(500) Ne 7024.05 7024.05(1000) Ne 7032.413 7032.413 1 1 1 1 1 1 1 1 1 11 Ar 7147.041 7147.041 7147.041 130 Ne 7173.938 7173.938 7173.938 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 160 Ne 7245.166 7245.166 7245.166 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1(1000) Cd 7345.671 Ar 7383.98 7383.98 7383.98 1 1 1 1 1 130 Ne 7438.898 7438.898 7438.898 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 110 Ne 7488.871 7488.871 7488.871 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 11 Ar 7503.867 7503.867 7503.867 11 Ar 7514.651 7514.651 7514.651 1 1 1(300) Ne 7535.774 7535.774 1 1 1 1(100) Ne 7544.044 7544.0441 Ar 7635.105 7635.105 7635.105 1 1 1 1 1 1 1 1 1 1 1 1 11 ? 7645 7645 76451 ? 7724.628 7724.628 7724.628 1 1 1(200) Ne 7943.18 7943.18 1 1 1 1 1 1 1 1 11 Ar 7948.175 7948.175 7948.1751 (????)Ne 8082.457 8082.457 8082.4571 Ar 8103.692 8103.692 8103.6921 Ar 8115.311 8115.311 8115.311 1 1 1 1 1 1 1 1 1 1 1(300) Ne 8136.406 8136.406 1 1 1 1 1 1 1 15 ? 8263 8263 1 11 Ar 8264.521 8264.521 8264.521 1 1 1 1 1 1 140 Ne 8300.324 8300.324 8300.324 1 1 1 1 1 1 1 1 1 1 1 1 170 Ne 8377.606 8377.606 8377.606 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 120 Ne 8418.426 8418.426 8418.426 1 1 1 1 1 1 1 11 Ar 8424.647 8424.647 8424.647100 Ne 8495.359 8495.359 8495.359 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 1 11 Ar 8521.441 8521.441 8521.441 1

61 46 36 41 38 40 42 32 41 44 38 43 28 29 30 29 30 29 31 30 30 29

The RUNZ list omits some useful Ne lines. Argon lines are included even though this is not an argon lamp. We should possibly pick up the cadmium line at 7345 IRAF RUNZ Line lists

and matched lines in dispersion functions

Red: neon lines to be added

Blue: 6dfdr desert

IRAF 6dFDR

13

Arc spectrum R - HgCdNe

14

Arc spectrum V - HgCdHe

Not enough lines in high-

dispersion data to be used for

Dn- measurements

? Even with extra

lines from NIST ASD, still only 16 good lines

15

Agreement: batch x-cor results V data, R data and VR data compared z ≤ 0.0005 (150 km/s) out of 109 spectra

45

69 78

RUNZ R RUNZ V

RUNZ VR

43IRAF R 57

16

RUNZ-VR misidentifications 11/109

V 21/109; R 28/109 z = ~ 0.09

17

R data: 109 galaxies - r-h plots from both x-correlations- “disagrees” are low S/N spectra

RUNZ: height and r-value of x-cor

0

5

10

15

20

25

30

35

0 0.2 0.4 0.6 0.8

h

r

Agree Disagree

IRAF: height and r-value of x-cor

0

5

10

15

20

25

30

0 0.2 0.4 0.6 0.8 1

h

r

Agree Disagree

Data from: IRAF – xcsao.log; RUNZ – read from display (r writes to log)

18

Mean uncertainty in x-correlation 109 galaxies

RUNZ R ± 79 km/s

(z ± 0.0003)

RUNZ V ± 84 km/s

(z ± 0.0003)

RUNZ VR ± 59 km/s

(z ± 0.0002)

IRAF R ± 41 km/s

(z ± 0.0001)Data from: IRAF – xcsao.log; RUNZ – verr from 0924Rcom.sdfz.zlog

IRAF uses 12 templates, RUNZ uses 8 templates

19

X-correlation R data 57 well-matched galaxies

Error bars are x-correlation uncertainties

Z-Z analysis: R data y = 1.0013x - 0.0002

R2 = 0.9999

-0.01

0.00

0.01

0.02

0.03

0.04

0.05

0.06

0.07

0.08

-0.01 0 0.01 0.02 0.03 0.04 0.05 0.06 0.07 0.08

IRAF redshifts

RU

NZ

re

ds

hif

ts

20

X-correlation R data All 109 galaxies

Z-Z analysis: R data

-0.05

0

0.05

0.1

0.15

-0.15 -0.1 -0.05 0 0.05 0.1 0.15 0.2 0.25 0.3

IRAF redshift

RU

NZ

red

shif

t

21

Line Measurements – 9 galaxies

Z-Z analysis: R data y = 1.0138x - 0.0006

R2 = 0.9995

0

0.02

0.04

0.06

0.08

0.1

0.12

0.14

0.00 0.02 0.04 0.06 0.08 0.10 0.12 0.14

IRAF redshifts

RU

NZ

re

ds

hif

ts

22

Summary Results S/N appears higher in RUNZ than in IRAF Line lists should be reviewed 6dFDR should have “retain all lines” option Update all versions of RUNZ to do heliocentric correction

properly Can’t batch-process

– still need to check for misidentifications Disagreements between methods and gratings on low

S/N data not a matter of concern X-cor uncertainty could be quoted on RUNZ screen

display and should be mentioned in online database May reduce uncertainty by including more templates for

RUNZ Overall z values concur in cases of proper identification … and keep in mind …

23

Results from these analyses are preliminary! Many more fields will be studied VPH grating data will be compared with

reflection grating data Repeatability of measurements will be

tested on repeat observation if possible

24

Thanks

Anglo-Australian Observatory Wide-Field Astronomy Unit, Edinburgh Macquarie University

6df Galaxy Survey Team (37 members) Will Saunders, AAO Quentin Parker, MU/AAO