GAMA-09 master catalogue¶
Preparation of Pan-STARRS1 - 3pi Steradian Survey (3SS) data¶
This catalogue comes from dmu0_PanSTARRS1-3SS.
In the catalogue, we keep:
- The
uniquePspsSTidas unique object identifier; - The r-band position which is given for all the sources;
- The grizy
<band>FApMagaperture magnitude (see below); - The grizy
<band>FKronMagas total magnitude.
The Pan-STARRS1-3SS catalogue provides for each band an aperture magnitude defined as “In PS1, an 'optimal' aperture radius is determined based on the local PSF. The wings of the same analytic PSF are then used to extrapolate the flux measured inside this aperture to a 'total' flux.”
The observations used for the catalogue where done between 2010 and 2015 (ref).
In [1]:
from herschelhelp_internal import git_version
print("This notebook was run with herschelhelp_internal version: \n{}".format(git_version()))
In [2]:
%matplotlib inline
#%config InlineBackend.figure_format = 'svg'
import matplotlib.pyplot as plt
plt.rc('figure', figsize=(10, 6))
from collections import OrderedDict
import os
from astropy import units as u
from astropy.coordinates import SkyCoord
from astropy.table import Column, Table
import numpy as np
from herschelhelp_internal.flagging import gaia_flag_column
from herschelhelp_internal.masterlist import nb_astcor_diag_plot, remove_duplicates
from herschelhelp_internal.utils import astrometric_correction, mag_to_flux
In [3]:
OUT_DIR = os.environ.get('TMP_DIR', "./data_tmp")
try:
os.makedirs(OUT_DIR)
except FileExistsError:
pass
RA_COL = "ps1_ra"
DEC_COL = "ps1_dec"
I - Column selection¶
In [4]:
imported_columns = OrderedDict({
"objID": "ps1_id",
"raMean": "ps1_ra",
"decMean": "ps1_dec",
"gFApMag": "m_ap_gpc1_g",
"gFApMagErr": "merr_ap_gpc1_g",
"gFKronMag": "m_gpc1_g",
"gFKronMagErr": "merr_gpc1_g",
"rFApMag": "m_ap_gpc1_r",
"rFApMagErr": "merr_ap_gpc1_r",
"rFKronMag": "m_gpc1_r",
"rFKronMagErr": "merr_gpc1_r",
"iFApMag": "m_ap_gpc1_i",
"iFApMagErr": "merr_ap_gpc1_i",
"iFKronMag": "m_gpc1_i",
"iFKronMagErr": "merr_gpc1_i",
"zFApMag": "m_ap_gpc1_z",
"zFApMagErr": "merr_ap_gpc1_z",
"zFKronMag": "m_gpc1_z",
"zFKronMagErr": "merr_gpc1_z",
"yFApMag": "m_ap_gpc1_y",
"yFApMagErr": "merr_ap_gpc1_y",
"yFKronMag": "m_gpc1_y",
"yFKronMagErr": "merr_gpc1_y"
})
catalogue = Table.read("../../dmu0/dmu0_PanSTARRS1-3SS/data/PanSTARRS1-3SS_GAMA-09_v2.fits")[list(imported_columns)]
for column in imported_columns:
catalogue[column].name = imported_columns[column]
epoch = 2012
# Clean table metadata
catalogue.meta = None
In [5]:
# Adding flux and band-flag columns
for col in catalogue.colnames:
if col.startswith('m_'):
errcol = "merr{}".format(col[1:])
# -999 is used for missing values
catalogue[col][catalogue[col] < -900] = np.nan
catalogue[errcol][catalogue[errcol] < -900] = np.nan
flux, error = mag_to_flux(np.array(catalogue[col]), np.array(catalogue[errcol]))
# Fluxes are added in µJy
catalogue.add_column(Column(flux * 1.e6, name="f{}".format(col[1:])))
catalogue.add_column(Column(error * 1.e6, name="f{}".format(errcol[1:])))
# Band-flag column
if "ap" not in col:
catalogue.add_column(Column(np.zeros(len(catalogue), dtype=bool), name="flag{}".format(col[1:])))
# TODO: Set to True the flag columns for fluxes that should not be used for SED fitting.
In [6]:
catalogue[:10].show_in_notebook()
Out[6]:
II - Removal of duplicated sources¶
We remove duplicated objects from the input catalogues.
In [7]:
SORT_COLS = ['merr_ap_gpc1_r', 'merr_ap_gpc1_g', 'merr_ap_gpc1_i', 'merr_ap_gpc1_z', 'merr_ap_gpc1_y']
FLAG_NAME = 'ps1_flag_cleaned'
nb_orig_sources = len(catalogue)
catalogue = remove_duplicates(catalogue, RA_COL, DEC_COL, sort_col=SORT_COLS, flag_name=FLAG_NAME)
nb_sources = len(catalogue)
print("The initial catalogue had {} sources.".format(nb_orig_sources))
print("The cleaned catalogue has {} sources ({} removed).".format(nb_sources, nb_orig_sources - nb_sources))
print("The cleaned catalogue has {} sources flagged as having been cleaned".format(np.sum(catalogue[FLAG_NAME])))
III - Astrometry correction¶
We match the astrometry to the Gaia one. We limit the Gaia catalogue to sources with a g band flux between the 30th and the 70th percentile. Some quick tests show that this give the lower dispersion in the results.
In [8]:
gaia = Table.read("../../dmu0/dmu0_GAIA/data/GAIA_GAMA-09.fits")
gaia_coords = SkyCoord(gaia['ra'], gaia['dec'])
In [9]:
nb_astcor_diag_plot(catalogue[RA_COL], catalogue[DEC_COL],
gaia_coords.ra, gaia_coords.dec)
In [10]:
delta_ra, delta_dec = astrometric_correction(
SkyCoord(catalogue[RA_COL], catalogue[DEC_COL]),
gaia_coords
)
print("RA correction: {}".format(delta_ra))
print("Dec correction: {}".format(delta_dec))
In [11]:
catalogue[RA_COL] += delta_ra.to(u.deg)
catalogue[DEC_COL] += delta_dec.to(u.deg)
In [12]:
nb_astcor_diag_plot(catalogue[RA_COL], catalogue[DEC_COL],
gaia_coords.ra, gaia_coords.dec)
IV - Flagging Gaia objects¶
In [13]:
catalogue.add_column(
gaia_flag_column(SkyCoord(catalogue[RA_COL], catalogue[DEC_COL]), epoch, gaia)
)
In [14]:
GAIA_FLAG_NAME = "ps1_flag_gaia"
catalogue['flag_gaia'].name = GAIA_FLAG_NAME
print("{} sources flagged.".format(np.sum(catalogue[GAIA_FLAG_NAME] > 0)))
V - Flagging objects near bright stars¶
VI - Saving to disk¶
In [15]:
catalogue.write("{}/PS1.fits".format(OUT_DIR), overwrite=True)