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‎DP1/300_Science_Demos/309_Astronomical_analysis/309_2_convert_between_photometric_systems.ipynb‎

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"Data Release: <a href=\"https://dp1.lsst.io/\">Data Preview 1</a>\\\n",
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"Container Size: medium\\\n",
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"LSST Science Pipelines version: v29.2.0\\\n",
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"Last verified to run: 2026-02-10\\\n",
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"Last verified to run: 2026-03-24\\\n",
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"Repository: [github.com/lsst/tutorial-notebooks](https://github.com/lsst/tutorial-notebooks)\\\n",
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"DOI: [10.11578/rubin/dc.20250909.20](https://doi.org/10.11578/rubin/dc.20250909.20)"
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"\n",
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"Two methods for transforming between photometric systems are explored in <a href=\"https://rtn-099.lsst.io/\">RTN-099</a>: polynomial relations and lookup tables. The guiding principle for which is to use is driven by the balance between simplicity and accuracy: in general, simple first- or second-order polynomials are sufficient, but, for higher accuracy, one may instead choose the slightly more difficult-to-employ lookup-table method.\n",
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"\n",
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"This tutorial demonstrates how to apply both methods of photometric transformation. Examples are provided for converting from Rubin DP1 $i$-band photometry to PanSTARRS1 DR2 and DES DR2 $i$ bands, and from Rubin DP1 $g$-band photometry to Gaia DR3 $RP$-band photometry.\n",
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"This tutorial demonstrates how to apply both methods of photometric transformation. Examples are provided for converting from Rubin DP1 $i$-band photometry to PanSTARRS1 DR2 and DES DR2 $i$ bands, and from Rubin DP1 $g$-band photometry to Gaia DR3 $BP$-band photometry.\n",
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"\n",
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"**Related tutorials:** The 100-level tutorials demonstrate how to use the butler, the TAP service, and the Firefly image display. The 200-level tutorials introduce the types of image and catalog data.\n"
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]
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{
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"cell_type": "markdown",
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"id": "686c2789-0b71-4bc4-b15b-0b020a0d965f",
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"metadata": {},
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"metadata": {
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"execution": {
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"iopub.execute_input": "2025-10-17T18:50:22.291274Z",
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}
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},
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"source": [
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"Calculate color indices using the PSF magnitudes, and plot a color-color diagram. Color-code points by the $r$-band PSF magnitude error."
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]
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{
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"cell_type": "markdown",
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"id": "e3e1fe82-cea3-4cc2-81d6-5e9310d2ced1",
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"metadata": {},
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"metadata": {
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},
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"source": [
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"\n",
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"| Conversion | Transformation Equation | RMS | Applicable Color Range | QA Plot |\n",
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{
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"cell_type": "markdown",
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"id": "c4f941a7-2394-4dd9-b2cf-ce5fb16f8395",
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"metadata": {},
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"metadata": {
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"execution": {
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"iopub.execute_input": "2025-12-19T23:32:23.571408Z",
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}
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},
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"source": [
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"Use the `cross_match_catalogs` function defined above to match the two catalogs based on the stars' coordinates."
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]
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{
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"cell_type": "markdown",
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"id": "8623e190-aa85-4dd0-b186-88e19483743f",
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"metadata": {},
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"metadata": {
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"execution": {
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}
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},
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"source": [
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"### 3.3.3 Compare the LSSTComCam-estimated PS1 i-band magnitudes with the PanSTARRS1 DR2 i-band magnitudes"
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{
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"cell_type": "markdown",
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"id": "0570b618-901f-4c60-bd32-17ea8d69c99f",
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"metadata": {},
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"metadata": {
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"execution": {
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}
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},
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"source": [
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"## 4. Piecewise 1st-order polynomial transformation: LSSTComCam $i$ --> DES DR2 $i$\n",
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"\n",
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{
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"cell_type": "markdown",
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"id": "35075b43-4e76-4463-a359-def323fa8520",
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"metadata": {},
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"metadata": {
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"execution": {
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"iopub.execute_input": "2025-12-05T20:10:17.123399Z",
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}
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},
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"source": [
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"![Alt text](https://rtn-099.lsst.io/_downloads/0d5bd60339db84127abb8bd0f7b096e0/qaPlot.ComCam_to_DESDR2_ECDFS.fit.dmag_i_des-i_ComCam.gi_ComCam.norder1.qa1.png)\n",
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"\n",
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"id": "939e52ad-9ce0-45eb-a163-bb9ad9467df8",
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"metadata": {},
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"source": [
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"Here are the quality assurance (QA) plots from <a href=\"https://rtn-099.lsst.io/\">RTN-099</a> associated with the second-order polynomial fit of the DP1 $g$-band to Gaia DR3 $RP$-band. Note from the bottom-right plot that a third-order term might benefit the fit, but staying with the simpler second-order polynomial still achieves a 0.027 mag RMS in the fit. For more accuracy, using the lookup table method (described in the next section) is recommended."
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"Here are the quality assurance (QA) plots from <a href=\"https://rtn-099.lsst.io/\">RTN-099</a> associated with the second-order polynomial fit of the DP1 $g$-band to Gaia DR3 $BP$-band. Note from the bottom-right plot that a third-order term might benefit the fit, but staying with the simpler second-order polynomial still achieves a 0.027 mag RMS in the fit. For more accuracy, using the lookup table method (described in the next section) is recommended."
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]
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},
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{
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"id": "10f38f41-8bec-418e-a778-18246278f130",
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"metadata": {},
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"source": [
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"Test the transformation by comparing the Gaia DR3 $RP$-band magnitudes estimated from the DP1 data in ECDFS against the Gaia DR3 $RP$-band magnitudes from the Gaia DR3 data themselves in ECDFS."
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"Test the transformation by comparing the Gaia DR3 $BP$-band magnitudes estimated from the DP1 data in ECDFS against the Gaia DR3 $BP$-band magnitudes from the Gaia DR3 data themselves in ECDFS."
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]
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},
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{
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"id": "febf7500-a25f-4209-b337-86108f4f4d6c",
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"metadata": {},
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"source": [
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"Calculate both the differences between the DP1 $g$-band magnitude and the Gaia DR3 $RP$-band magnitude (\"before transformation\") and the differences between DP1-estimated Gaia DR3 $RP$-band magnitude and the actual Gaia DR3 $RP$-band magnitude (\"after transformation\"):"
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"Calculate both the differences between the DP1 $g$-band magnitude and the Gaia DR3 $BP$-band magnitude (\"before transformation\") and the differences between DP1-estimated Gaia DR3 $BP$-band magnitude and the actual Gaia DR3 $BP$-band magnitude (\"after transformation\"):"
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]
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},
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{
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"id": "3581e642-4b84-4cc9-b898-be00f0846653",
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"metadata": {},
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"source": [
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"Here are the quality‑assurance (QA) plots from <a href=\"https://rtn-099.lsst.io/\">RTN-099</a> that document the lookup‑table transformation from the DP1 $g$‑band to the Gaia DR3 $RP$‑band. The lookup table is constructed by binning matched stars in the ECDFS field by their Rubin DP1 $(g–i)$ color, and then tabulating the median magnitude offset between the Gaia DR3 RP‑band and the Rubin DP1 g‑band for the stars in each color bin."
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"Here are the quality‑assurance (QA) plots from <a href=\"https://rtn-099.lsst.io/\">RTN-099</a> that document the lookup‑table transformation from the DP1 $g$‑band to the Gaia DR3 $BP$‑band. The lookup table is constructed by binning matched stars in the ECDFS field by their Rubin DP1 $(g–i)$ color, and then tabulating the median magnitude offset between the Gaia DR3 RP‑band and the Rubin DP1 g‑band for the stars in each color bin."
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]
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},
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{
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"cell_type": "code",
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"execution_count": null,
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"id": "d6f731f9-1084-46fc-a881-80a62b241dd8",
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"metadata": {},
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"metadata": {
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"scrolled": true
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},
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"outputs": [],
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"source": [
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"df_lut = pd.read_csv(lut_url)\n",
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"id": "376a20fd-2f9c-4005-9782-6d8607d59d72",
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"metadata": {},
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"source": [
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"Test the transformation by comparing the Gaia DR3 $RP$-band magnitudes estimated from the DP1 data in ECDFS against the Gaia DR3 $RP$-band magnitudes from the Gaia DR3 data themselves."
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"Test the transformation by comparing the Gaia DR3 $BP$-band magnitudes estimated from the DP1 data in ECDFS against the Gaia DR3 $BP$-band magnitudes from the Gaia DR3 data themselves."
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]
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},
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{
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"plt.grid(True)\n",
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"plt.grid(color='grey')\n",
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"plt.legend(loc='upper left', fontsize=8)\n",
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"plt.title(r\"mag difference between LSSTComCam DP1 $g$-band (and transformed $BP$-band) and Gaia DR3 $RP$-band\")\n",
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"plt.title(r\"mag difference between LSSTComCam DP1 $g$-band (and transformed $BP$-band) and Gaia DR3 $BP$-band\")\n",
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"plt.show()"
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]
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},

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