Production version of the Input Catalog (+ Pilot survey...

Zwitter, Sydney, 3-feb-2014

Production version of the Input Catalog(+ Pilot survey projects)

Fixing small inconsistencies, so everything re-done from scratch (sic!).

All information contained in the original catalogs (2MASS, UCAC4, APASS DR7) is now contained in our input catalog.

The problem of proper motions solved: we go for the UCAC4 coordinates and proper motions and not for the PPMXL ones as before.

This decision has been justified by comparison of independent catalogs (UCAC4 ↔ APASS and PPMXL ↔ APASS). Also cluster PMs support that.

In a nutshell, the final decision train: Sources selected from 2MASS (we know its point source catalog objects with

"good" flags are real stars, not double identifications, asteroids, CCD errors, etc.). Astrometry comes from UCAC4, the best and most reliable astrometric catalog in our magnitude range. Photometry comes from APASS DR7, the only photometric measurements in our wavelengths which are accurate and nearly complete. To be supplemented with DR8 within one year.


Input Catalog: fixing small inconsistencies

we start with 2mass PSC catalog. First we pick up stars with:

photometric quality flag (Q) = 'A' for J and K bands, photometry estimation method flag (R) with value 1, 2, or 3 for J and K bands, blend flag (B) = 1 for J and K bands contamination and confusion flag (C) = 0 for J and K bands, extended source contamination flag (X) = 0, minor planet flag (A) = 0.

We also require that |b| ≥ 5.0o and δ ≤ 10o (a tiny bug in Galactic coordinates fixed here).

We still estimate V magnitude from the formula V = K + 2.0 (J-K+0.14)+0.382 e(J-K-0.2)/0.5

but we now require that 0.0 < V < 14.3 (the limit in previous editions of the catalog was 14.0).

Equinox of 2MASSS, UCAC4, PPMXL, and APASS is J2000, but epoch is not. Cross-identification to UCAC4 is done matching the value of pts2key in both catalogs.

Cross-identification to APASS DR7 is done by forwarding UCAC4 coordinates to epoch 2011 and then by picking the closest match which has APASS coordinates and which is within <10".


Input Catalog: complenetess, in a nutshell

8.149.211 (100%) objects with V<14.3 in 2MASS,

from these:

577 (0.007%) 2MASS objects missing in UCAC4,

743400 (9.12%) 2MASS objects missing in APASS DR7, a large fraction of them in consecutive regions.


Input Catalog: V < 14 stars affected by bright neighbours of a given V magnitude

avoid-ance

5o-7o 7o-10o 10o-15o 15o-20o 20o-25o 25o-50o 50o-90o SUM

1 - 2 115" 0 7 0 1 0 0 0 8

2 - 3 105" 6 8 7 4 6 5 4 40

3 - 4 95" 7 8 17 10 12 10 6 70

4 - 5 85" 19 28 38 14 19 23 17 158

5 - 6 75" 50 56 67 64 34 77 26 374

6 - 7 65" 92 154 144 80 55 128 45 698

7 - 8 55" 159 159 194 122 92 193 78 997

8 - 9 45" 475 652 701 485 274 624 237 3448

9 - 10 35" 1657 2127 2308 1327 873 1827 751 10870

10 - 11 25" 2550 3053 3328 1710 1136 2388 894 15059

11 - 12 15" 3012 3369 3464 1875 1180 2432 949 16281

12 - 13 5" 891 971 991 494 292 711 269 4619

SUM 8918 10592 11259 6186 3973 8418 3276 52622

───── Distance from the Galactic plane ─────

──

──

──

V m

agni

tude

ran

ge ─

──

──

──

─Similar to work of Jeffrey Simpson


Input Catalog: selection based on 2MASS: its epoch


Input Catalog: comparison of positions in 2MASS and UCAC4


Input Catalog: UCAC4 (epoch 2000): size of proper motions

V < 14.3, |b| > 5o, δ < +10o.


Input Catalog: Accuracy of positions of APASS DR7 (epoch ~2011)


Input Catalog: UCAC4 moved to epoch 2011 and compared to APASS DR7


Input Catalog: PPMXL moved to epoch 2011 and compared to APASS DR7

This is worse than UCAC4!


Proper motion for clusters: not trivialBellini et al. 2010: M67


Proper motion for clusters: not trivial Simon Murphy et al. 2013: ε Cha


Input Catalog: proper motions in clusters: PPMXL and UCAC4

PM grouping of cluster members around the cluster's PM (red cross) seen in UCAC4, not in PPMXL.


Input Catalog: proper motions in clusters: PPMXL and UCAC410% of ppmxl star plotted

PPMXL is larger (only 10% of the objects plotted in the right panels) but not as accurate.


Input Catalog: APASS V magnitude compared to the one predicted from 2MASS

V magnitude match is reasonable, but not perfect. Errors of ~0.35 mag present in ~10% of the cases.


Census

V(faint) max(|b|) |b| > 5o |b| > 6o |b| > 7o |b| > 8o |b| > 9o |b| > 10o

13.0 19 1.178.171 1.070.008 965.782 864.906 767.633 671.756

13.25 23 1.739.235 1.601.753 1.468.973 1.340.505 1.216.432 1.094.288

13.5 28 2.477.208 2.304.400 2.136.953 1.975.426 1.818.606 1.664.687

13.75 31 3.245.985 3.031.454 2.823.245 2.621.419 2.425.818 2.233.851

14.0 32 4.045.208 3.771.433 3.515.707 3.267.928 3.026.891 2.790.816

Number of APASS stars in fields with >450 stars per FOV, with V > 10 and without bright neighbours.


Conclusions on the Input Catalog

Fixing small inconsistencies, so everything re-done from scratch (sic!).

All information contained in the original catalogs (2MASS, UCAC4, APASS DR7) is now contained in our input catalog.

The problem of proper motions solved: we go for the UCAC4 coordinates and proper motions and not for the PPMXL ones as before.

This decision has been justified by comparison of independent catalogs (UCAC4 ↔ APASS and PPMXL ↔ APASS).

In a nutshell, the final decision train: Sources selected from 2MASS (we know its point source catalog objects with

"good" flags are real stars, not double identifications, asteroids, CCD errors, etc.). Astrometry comes from UCAC4, the best and most reliable astrometric catalog in our magnitude range. Photometry comes from APASS DR7, the only photometric measurements in our wavelengths which are accurate and nearly complete. To be supplemented with DR8 within one year.


Peculiar stars and ISM

ISM: rich possibilities on DIBs.

A paper by Kos et al. on RAVE to be circulated soon.

Peculiars: Gaia-ESO also covers Hα.

Many clusters covered.

We found 1323 spectra (out of 11.076 observed) with Hα in emission.

Close to 50% of emission spectra have composed Hα profiles.


Hα profile decomposition


Conclusions on ISM and peculiar objects

A paper on EW of diffuse interstellar bands (there are many in Galah data!) and a paper on a discovery of emission type objects (Hα,β) can be done in a few months.

But both require reliable reductions, in particular background (including Moonlight) subtraction.

Reliability of 2dfdr not demonstrated yet, so we should be able to cross-check. Raw data are nicely available, but could you post a spectral tracing with identifications of ThXe lamp lines on the wiki?

Production version of the Input Catalog (+ Pilot survey...

Documents

Transcript of Production version of the Input Catalog (+ Pilot survey...