from astropy import units as u

u.m

u.Angstrom

print(u.m.__doc__)

print(u.m.physical_type)

print(u.Angstrom.physical_type)

1.0 * u.m

[1.0, 2.0, 3.0] * u.m

q = [1.0, 2.0, 3.0] * u.m
q.to(u.Angstrom)

q1 = 3. * u.m

q1

q2 = 5. * u.cm / u.s / u.g**2

q2

q1 * q2

(q1 * q2).to(u.m**2 / u.kg**2 / u.s)

from astropy.constants import G

print repr(G)

F = (G * 1. * u.M_sun * 100. * u.kg) / (3.2 * u.au)**2

F.unit.find_equivalent_units()

F.to(u.N)

(450. * u.nm).to(u.GHz)

(450. * u.nm).to(u.GHz, equivalencies=u.spectral())

(450. * u.eV).to(u.nm, equivalencies=u.spectral())

import numpy as np
np.sin(90)

np.sin(90 * u.degree)

from astropy.table import Table
import numpy as np

t = Table()
t['name'] = ['source 1', 'source 2', 'source 3', 'source 4']
t['flux'] = [1.2, 2.2, 3.1, 4.3]

t.colnames

t.dtype

t

t.show_in_browser()

t['flux']

t[1]

t[1:3]

t2 = Table([['x', 'y', 'z'], 
            [1.1, 2.2, 3.3]],
           names=['name', 'value'],
           masked=True)
t2

t2['value'].mask = [False, True, False]

t2

t2['value'].mean()

t2['value'].fill_value

t2['value'].fill_value = -99

t2.filled()

t

t2 = Table()
t2['name'] = ['source 1', 'source 3', 'source 8']
t2['flux2'] = [1.4, 3.5, 8.6]

from astropy.table import join
t3 = join(t, t2, keys=['name'], join_type='outer')
t3

t3 = join(t, t2, keys=['name'], join_type='inner')
t3

t3.write('example.fits', overwrite=True)

t4 = Table.read('example.fits')

t4

t4.write('example.vot', format='votable', overwrite=True)

!cat example.vot

t = Table()
t['name'] = ['source 1', 'source 2', 'source 3', 'source 4']
t['flux'] = [1.2, 2.2, 3.1, 4.3]

t

t.write('mytable.tex', format='latex')

t.write(sys.stdout, format='latex')

text = """
\begin{table}
\begin{tabular}{cc}
name & flux \\
source 1 & 1.2 \\
source 2 & 2.2 \\
source 3 & 3.1 \\
source 4 & 4.3 \\
\end{tabular}
\end{table}
"""

Table.read('mytable.tex', format='latex')

import sys
sys.stdout

from astropy.io import fits

# The following FITS file lives in the lesson repository, relative
# to this file.  However, if you get a "file not found" error you can download and open the file
# by uncommenting these lines (and commenting the last line)

# from astropy.utils import download_file
# filename = download_file('https://github.com/abostroem/2015-01-03-aas/raw/gh-pages/intermediate/astropy/data/gll_iem_v02_P6_V11_DIFFUSE.fit')
# hdulist = fits.open(filename)
hdulist = fits.open('data/gll_iem_v02_P6_V11_DIFFUSE.fit')

hdulist.info()

primary_hdu = hdulist[0]

primary_hdu = hdulist['PRIMARY']

primary_hdu.header

primary_hdu.header['OBSERVER']

primary_hdu.header['DATE']

%matplotlib inline
from matplotlib.pyplot import imshow

imshow(primary_hdu.data[0], origin='lower')

from aplpy import FITSFigure

fig = FITSFigure('data/gll_iem_v02_P6_V11_DIFFUSE.fit', slices=[0])
fig.show_colorscale()

new_hdu = fits.PrimaryHDU(data=primary_hdu.data[0], header=primary_hdu.header)

del new_hdu.header['FILENAME']

del new_hdu.header['C*3']

new_hdu.header

new_hdu.writeto('lat_background_model_slice.fits', checksum=True,
                clobber=True)

from astropy.coordinates import SkyCoord
from astropy import units as u

SkyCoord(ra=10.68458 * u.deg, dec=41.26917 * u.deg, frame='icrs')

c = SkyCoord('00h42m44.3s +41d16m9s', frame='icrs')
c

c.ra

c.ra.hour

c.galactic

c.transform_to('galactic')

from astropy.coordinates import FK5

FK5?

frame = FK5(equinox='J2010')

c.transform_to(frame)