4. Transformation and Selection

In the previous lesson, we identified stars with the proper motion we expect for GD-1.

Now we'll do the same selection in an ADQL query, which will make it possible to work with a larger region of the sky and still download less data.

Outline

Here are the steps in this lesson:

  1. Using data from the previous lesson, we'll identify the values of proper motion for stars likely to be in GD-1.

  2. Then we'll compose an ADQL query that selects stars based on proper motion, so we can download only the data we need.

That will make it possible to search a bigger region of the sky in a single query. We'll also see how to write the results to a CSV file.

After completing this lesson, you should be able to

  • Transform proper motions from one frame to another.

  • Compute the convex hull of a set of points.

  • Write an ADQL query that selects based on proper motion.

  • Save data in CSV format.

Installing libraries

If you are running this notebook on Colab, you can run the following cell to install the libraries we'll use.

If you are running this notebook on your own computer, you might have to install these libraries yourself. See the instructions in the preface.

In [37]:
# If we're running on Colab, install libraries

import sys
IN_COLAB = 'google.colab' in sys.modules

if IN_COLAB:
    !pip install astroquery astro-gala

Reload the data

You can download the data from the previous lesson or run the following cell, which downloads it if necessary.

In [38]:
from os.path import basename, exists

def download(url):
    filename = basename(url)
    if not exists(filename):
        from urllib.request import urlretrieve
        local, _ = urlretrieve(url, filename)
        print('Downloaded ' + local)

download('https://github.com/AllenDowney/AstronomicalData/raw/main/' +
         'data/gd1_data.hdf')

Now we can reload centerline_df and selected_df.

In [39]:
import pandas as pd

filename = 'gd1_data.hdf'
centerline_df = pd.read_hdf(filename, 'centerline_df')
selected_df = pd.read_hdf(filename, 'selected_df')

Selection by proper motion

Let's review how we got to this point.

  1. We made an ADQL query to the Gaia server to get data for stars in the vicinity of GD-1.

  2. We transformed the coordinates to the GD1Koposov10 frame so we could select stars along the centerline of GD-1.

  3. We plotted the proper motion of the centerline stars to identify the bounds of the overdense region.

  4. We made a mask that selects stars whose proper motion is in the overdense region.

At this point we have downloaded data for a relatively large number of stars (more than 100,000) and selected a relatively small number (around 1000).

It would be more efficient to use ADQL to select only the stars we need. That would also make it possible to download data covering a larger region of the sky.

However, the selection we did was based on proper motion in the GD1Koposov10 frame. In order to do the same selection in ADQL, we have to work with proper motions in ICRS.

As a reminder, here's the rectangle we selected based on proper motion in the GD1Koposov10 frame.

In [40]:
pm1_min = -8.9
pm1_max = -6.9
pm2_min = -2.2
pm2_max =  1.0
In [41]:
def make_rectangle(x1, x2, y1, y2):
    """Return the corners of a rectangle."""
    xs = [x1, x1, x2, x2, x1]
    ys = [y1, y2, y2, y1, y1]
    return xs, ys
In [42]:
pm1_rect, pm2_rect = make_rectangle(
    pm1_min, pm1_max, pm2_min, pm2_max)

Since we'll need to plot proper motion several times, we'll use the following function.

In [43]:
import matplotlib.pyplot as plt

def plot_proper_motion(df):
    """Plot proper motion.
    
    df: DataFrame with `pm_phi1` and `pm_phi2`
    """
    x = df['pm_phi1']
    y = df['pm_phi2']
    plt.plot(x, y, 'ko', markersize=0.3, alpha=0.3)

    plt.xlabel('Proper motion phi1 (GD1 frame)')
    plt.ylabel('Proper motion phi2 (GD1 frame)')

    plt.xlim(-12, 8)
    plt.ylim(-10, 10)

The following figure shows:

  • Proper motion for the stars we selected along the center line of GD-1,

  • The rectangle we selected, and

  • The stars inside the rectangle highlighted in green.

In [44]:
plot_proper_motion(centerline_df)

plt.plot(pm1_rect, pm2_rect)

x = selected_df['pm_phi1']
y = selected_df['pm_phi2']
plt.plot(x, y, 'gx', markersize=0.3, alpha=0.3);

Now we'll make the same plot using proper motions in the ICRS frame, which are stored in columns pmra and pmdec.

In [45]:
x = centerline_df['pmra']
y = centerline_df['pmdec']
plt.plot(x, y, 'ko', markersize=0.3, alpha=0.3)

x = selected_df['pmra']
y = selected_df['pmdec']
plt.plot(x, y, 'gx', markersize=1, alpha=0.3)
    
plt.xlabel('Proper motion ra (ICRS frame)')
plt.ylabel('Proper motion dec (ICRS frame)')

plt.xlim([-10, 5])
plt.ylim([-20, 5]);

The proper motions of the selected stars are more spread out in this frame, which is why it was preferable to do the selection in the GD-1 frame.

But now we can define a polygon that encloses the proper motions of these stars in ICRS, and use that polygon as a selection criterion in an ADQL query.

Convex Hull

SciPy provides a function that computes the convex hull of a set of points, which is the smallest convex polygon that contains all of the points.

To use it, we'll select columns pmra and pmdec and convert them to a NumPy array.

In [46]:
import numpy as np

points = selected_df[['pmra','pmdec']].to_numpy()
points.shape

NOTE: If you are using an older version of Pandas, you might not have to_numpy(); you can use values instead, like this:

points = selected_df[['pmra','pmdec']].values

We'll pass the points to ConvexHull, which returns an object that contains the results.

In [47]:
from scipy.spatial import ConvexHull

hull = ConvexHull(points)
hull

hull.vertices contains the indices of the points that fall on the perimeter of the hull.

In [48]:
hull.vertices

We can use them as an index into the original array to select the corresponding rows.

In [49]:
pm_vertices = points[hull.vertices]
pm_vertices

To plot the resulting polygon, we have to pull out the x and y coordinates.

In [50]:
pmra_poly, pmdec_poly = np.transpose(pm_vertices)

This use of transpose is a useful NumPy idiom. Because pm_vertices has two columns, its matrix transpose has two rows, which are assigned to the two variables pmra_poly and pmdec_poly.

The following figure shows proper motion in ICRS again, along with the convex hull we just computed.

In [51]:
x = centerline_df['pmra']
y = centerline_df['pmdec']
plt.plot(x, y, 'ko', markersize=0.3, alpha=0.3)

x = selected_df['pmra']
y = selected_df['pmdec']
plt.plot(x, y, 'gx', markersize=0.3, alpha=0.3)

plt.plot(pmra_poly, pmdec_poly)
    
plt.xlabel('Proper motion phi1 (ICRS frame)')
plt.ylabel('Proper motion phi2 (ICRS frame)')

plt.xlim([-10, 5])
plt.ylim([-20, 5]);

So pm_vertices represents the polygon we want to select. The next step is to use it as part of an ADQL query.

Assembling the query

In Lesson 2 we used the following query to select stars in a polygonal region.

In [52]:
query5_base = """SELECT
{columns}
FROM gaiadr2.gaia_source
WHERE parallax < 1
  AND bp_rp BETWEEN -0.75 AND 2 
  AND 1 = CONTAINS(POINT(ra, dec), 
                   POLYGON({point_list}))
"""

In this lesson we'll make two changes:

  1. We'll select stars with coordinates in a larger region.

  2. We'll add another clause to select stars whose proper motion is in the polygon we just computed, pm_vertices.

Here are the coordinates of the larger rectangle in the GD-1 frame.

In [53]:
import astropy.units as u

phi1_min = -70 * u.degree
phi1_max = -20 * u.degree
phi2_min = -5 * u.degree
phi2_max = 5 * u.degree

We selected these bounds by trial and error, defining the largest region we can process in a single query.

In [54]:
phi1_rect, phi2_rect = make_rectangle(
    phi1_min, phi1_max, phi2_min, phi2_max)

Here's how we transform it to ICRS, as we saw in Lesson 2.

In [55]:
from gala.coordinates import GD1Koposov10
from astropy.coordinates import SkyCoord

gd1_frame = GD1Koposov10()
corners = SkyCoord(phi1=phi1_rect, 
                   phi2=phi2_rect, 
                   frame=gd1_frame)

corners_icrs = corners.transform_to('icrs')

To use corners_icrs as part of an ADQL query, we have to convert it to a string.
Here's the function from Lesson 2 we used to do that.

In [56]:
def skycoord_to_string(skycoord):
    """Convert SkyCoord to string."""
    t = skycoord.to_string()
    s = ' '.join(t)
    return s.replace(' ', ', ')
In [57]:
point_list = skycoord_to_string(corners_icrs)
point_list

Here are the columns we want to select.

In [58]:
columns = 'source_id, ra, dec, pmra, pmdec'

Now we have everything we need to assemble the query.

In [59]:
query5 = query5_base.format(columns=columns, 
                            point_list=point_list)
print(query5)

But don't try to run that query. Because it selects a larger region, there are too many stars to handle in a single query. Until we select by proper motion, that is.

Selecting proper motion

Now we're ready to add a WHERE clause to select stars whose proper motion falls in the polygon defined by pm_vertices.

To use pm_vertices as part of an ADQL query, we have to convert it to a string. Using flatten and array2string, we can almost get the format we need.

In [60]:
s = np.array2string(pm_vertices.flatten(), 
                    max_line_width=1000,
                    separator=',')
s

We just have to remove the brackets.

In [61]:
pm_point_list = s.strip('[]')
pm_point_list

Exercise

Define query6_base, starting with query5_base and adding a new clause to select stars whose coordinates of proper motion, pmra and pmdec, fall within the polygon defined by pm_point_list.

In [62]:
# Solution goes here

Exercise

Use format to format query6_base and define query6, filling in the values of columns, point_list, and pm_point_list.

In [63]:
# Solution goes here

Now we can run the query like this:

In [64]:
from astroquery.gaia import Gaia

job = Gaia.launch_job_async(query6)
print(job)

And get the results.

In [65]:
candidate_table = job.get_results()
len(candidate_table)

We call the results candidate_table because it contains stars that are good candidates for GD-1.

For the next lesson, we'll need point_list and pm_point_list again, so we should save them in a file. There are several ways we could do that, but since we are already storing data in an HDF file, let's do the same with these variables.

We've seen how to save a DataFrame in an HDF file. We can do the same thing with a Pandas Series. To make one, we'll start with a dictionary:

In [66]:
d = dict(point_list=point_list, pm_point_list=pm_point_list)
d

And use it to initialize a Series.

In [67]:
point_series = pd.Series(d)
point_series

Now we can save it in the usual way.

In [68]:
filename = 'gd1_data.hdf'
point_series.to_hdf(filename, 'point_series')

Plotting one more time

Let's see what the results look like.

In [69]:
x = candidate_table['ra']
y = candidate_table['dec']
plt.plot(x, y, 'ko', markersize=0.3, alpha=0.3)

plt.xlabel('ra (degree ICRS)')
plt.ylabel('dec (degree ICRS)');

Here we can see why it was useful to transform these coordinates. In ICRS, it is more difficult to identity the stars near the centerline of GD-1.

So let's transform the results back to the GD-1 frame. Here's the code we used to transform the coordinates and make a Pandas DataFrame, wrapped in a function.

In [70]:
from gala.coordinates import reflex_correct

def make_dataframe(table):
    """Transform coordinates from ICRS to GD-1 frame.
    
    table: Astropy Table
    
    returns: Pandas DataFrame
    """
    skycoord = SkyCoord(
               ra=table['ra'], 
               dec=table['dec'],
               pm_ra_cosdec=table['pmra'],
               pm_dec=table['pmdec'], 
               distance=8*u.kpc, 
               radial_velocity=0*u.km/u.s)

    gd1_frame = GD1Koposov10()
    transformed = skycoord.transform_to(gd1_frame)
    skycoord_gd1 = reflex_correct(transformed)

    df = table.to_pandas()
    df['phi1'] = skycoord_gd1.phi1
    df['phi2'] = skycoord_gd1.phi2
    df['pm_phi1'] = skycoord_gd1.pm_phi1_cosphi2
    df['pm_phi2'] = skycoord_gd1.pm_phi2
    return df

Here's how we use it:

In [71]:
candidate_df = make_dataframe(candidate_table)

And let's see the results.

In [72]:
x = candidate_df['phi1']
y = candidate_df['phi2']
plt.plot(x, y, 'ko', markersize=0.5, alpha=0.5)

plt.xlabel('phi1 (degree GD1)')
plt.ylabel('phi2 (degree GD1)');

We're starting to see GD-1 more clearly. We can compare this figure with this panel from Figure 1 from the original paper:

This panel shows stars selected based on proper motion only, so it is comparable to our figure (although notice that it covers a wider region).

In the next lesson, we will use photometry data from Pan-STARRS to do a second round of filtering, and see if we can replicate this panel.

Later we'll see how to add annotations like the ones in the figure and customize the style of the figure to present the results clearly and compellingly.

Summary

In the previous lesson we downloaded data for a large number of stars and then selected a small fraction of them based on proper motion.

In this lesson, we improved this process by writing a more complex query that uses the database to select stars based on proper motion. This process requires more computation on the Gaia server, but then we're able to either:

  1. Search the same region and download less data, or

  2. Search a larger region while still downloading a manageable amount of data.

In the next lesson, we'll learn about the database JOIN operation and use it to download photometry data from Pan-STARRS.

Best practices

  • When possible, "move the computation to the data"; that is, do as much of the work as possible on the database server before downloading the data.
In [ ]: