# 1.2.1. Star/galaxy/QSO classification¶

This science case starts from an imaging survey and takes steps toward classifying objects that are detected into stars, galaxies and quasi-stellar-objects (QSOs).

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## 1.2.1.1. Background¶

Imaging surveys encompass a number of different astronomical objects, generally including stars, galaxies and QSOs. Each category of objects is interesting in their own right, but not necessarily straightforward to classify. In particular, near the spatial resolution limit, compact galaxies, QSOs and stars may all appear as point sources.

In order to differentiate between these types of objects, work has been done extracting information from images such as photometry (magnitudes and colors) and/or the shape of light profiles. When available, spectroscopy can contribute more information thanks to spectral features (continuum shape, emission lines, absorption lines, etc.) and redshift information.

Here, we focus on the case where only imaging (photometry) is available.

## 1.2.1.2. Goal¶

We will investigate colors and model shapes (type) of astronomical objects in the DESI imaging Legacy Survey in order to classify them into stars, galaxies, and QSOs.

## 1.2.1.3. Data¶

We use DECam photometry, WISE photometry, and object type from the DECaLS DR3 catalog. Optical and infrared photometry is combined to plot bivariate distributions in color-color space.

DECam photometry includes the g, r, and z filters. WISE photometry is restricted to the more sensitive observations from the first two channels W1 and W2, respectively centered on 3.4 and 4.6 microns.

The object type can be one of these five: PSF, SIMP, EXP, DEV, COMP, as defined in the documentation.

Lastly, we retrieve postage stamp images from the DECaLS team Viewer tool using a set of URL’s and downloading/caching images.

## 1.2.1.4. Technique¶

The technique is to query the DECaLS Tractor catalog for photometric information including fluxes (to compute magnitudes), Milky Way transmission values (to correct for foreground extinction), and object model type (to have information on the shape of the light profile).

This information is then combined to separate population of points corresponding to object classes. Using color cuts for target selection or photometric identification is a common approach. We note that alternative approaches include using Machine Learning (e.g., Random Forest) in order to classify source types based on a training set of pre-classified objects.

## 1.2.1.5. Data Lab Workflow¶

The first steps are to import libraries that will be needed, and to authenticate.

Then, we query relevant columns from the tractor_primary view of the LS DR3 database. In this case, we query deredenned magnitudes g, r, z, W1, and W2 as well as the object type, and the RA and dec coordinates. We require a signal-to-noise ratio greater than 3 in each of the g, r, z bands.

query = """SELECT dered_mag_g as gmag, dered_mag_r as rmag,
dered_mag_z as zmag, dered_mag_w1 as w1mag, dered_mag_w2 as w2mag, type,
snr_g, snr_r, snr_z, ra, dec
FROM ls_dr3.tractor_primary
WHERE (snr_g>3 and snr_r>3 and snr_z>3)
LIMIT 100000"""


From the query results, we can plot color-color diagrams with any combination of colors. We select to combine optical and infrared colors, and look at both the population of objects overall, and split by object type. The RA and Dec coordinates will be used to retrieve a few image cutouts.

One could potentially extend this work by computing additional colors or using more information such as the magnitudes or goodness-of-fit of the model (chi squared values).

## 1.2.1.6. Output¶

The figure above shows structures in the bivariate distributions. In the top left panel, labeled ‘All’, we can see two branches that cross over each other, as well as a cloud of points below the branches. The remaining panels indicate that one of the branches corresponds to the stellar locus (PSF), while the other branch is a blend of galaxies with types SIMP, EXP, DEV & COMP. The cloud of points is a mixture of PSF, SIMP & EXP, perhaps including QSOs and compact galaxies. More work would be needed to confirm these classifications.