Adding v4.0 of thermal curve and changing filename in python too

jwst_backgrounds/jbt.py

@@ -54,7 +54,7 @@ def __init__(self, ra, dec, wavelength, thresh=1.1):
         self.cache_url = 'https://archive.stsci.edu/missions/jwst/simulations/straylight/sl_cache_2.0/'  # Path to the online location of the background cache
         self.local_path = os.path.join(os.path.dirname(__file__), 'refdata')
         self.wave_file = 'std_spectrum_wavelengths.txt'  # The wavelength grid of the background cache
-        self.thermal_file = 'thermal_curve_jwst_jrigby_v3.0.csv'  # The constant (not time variable) thermal self-emission curve
+        self.thermal_file = 'thermal_curve_jwst_jrigby_v4.0.csv'  # The constant (not time variable) thermal self-emission curve
         self.nside = 128  # Healpy parameter, from generate_backgroundmodel_cache.c .
         self.wave_array, self.thermal_bg = self.read_static_data()
         self.sl_nwave = self.wave_array.size  # Size of wavelength array

jwst_backgrounds/refdata/thermal_curve_jwst_jrigby_v4.0.csv

@@ -0,0 +1,378 @@
+#Title:    JWST thermal background spectrum to match backgrounds measured in Cycles 1 and 2
+#, Author:   Jane Rigby ([email protected])
+#, Date:     5 June 2024
+#, Version:  4.0
+#, Format:   comma separated variables (csv)
+#, Distribution:  unlimited (STI approval in NASA form 1675B.)
+#, Columns: wavelength (micron) and equivalent sky radiance (MJy/SR)
+#, 
+#, GENERATED BY: On-orbit thermal model-v3.ipynb.
+#, 
+#, SUMMARY: This is the self-emission thermal background spectrum for JWST,
+#, for use in planning observations.  At long wavelengths, self-emission
+#, from the observatory dominates over astrophysical backgrounds.
+#, 
+#, VERSION HISTORY: v1.X and v2.X were pre-launch predictions used to
+#, plan observations for Cycle 1.  v3.0 modifed that model to match
+#, thermal backgrounds as measured in commissioning (see Rigby, Lightsey
+#, et al. 2023, PASP, 135, 048002).
+#, 
+#, DESCRIPTION: Backgrounds were measured by the MIRI team at STScI, from
+#, all MIRI imaging observations taken between July 2022 and May 2024.
+#, Only observations with Ecliptic latitude >30 degree and Galactic
+#, latitude >30 degree were used.  For each broadband filter, the
+#, background versus time was plotted, and the data fit with two
+#, components: a linear component and a sinusoid with period 1 year and
+#, max at perihelion.  Since the MIRI backgrounds are slowly rising with
+#, time, for conservativism in observation planning for Cycle 4, the fits
+#, were extrapolated to perihelion (Jan 2026). This process determined
+#, the measured backgrounds for the MIRI imaging filters.
+#, 
+#, Since what is needed for observation planning is a thermal spectrum at
+#, all relevant wavelengths, not just at the centers of the MIRI imager
+#, filters, a physically-motivated model was fit to these data.  As in
+#, past versions, this simple model approximates JWST as a small number
+#, of components (in this case, 33), each represented by a single
+#, blackbody.  Detailed ray tracing before launch by Paul Lightsey
+#, predicted the effective radiances at 10, 15, 20, 25um micron from
+#, approximately twenty different components of JWST.
+#, (2019.12.03_MIR_summary.xlsx, dated Dec 3 2019, based on integrated
+#, thermal model v5.5u4b_EOL_0R_P52P_SL-LTO., which assumed perihelion,
+#, hot pitch, and end of life sunshield performance.)  For each
+#, component, we computed the temperature and effective area x emissivity
+#, of the blackbody that could produce those radiances.  See Rigby et
+#, al. (2023) for details. One can think of "effective area x emissivity"
+#, as how effectively the component scatters thermal emission into the
+#, JWST beam.
+#, 
+#, An improvement over previous versions is the treatment of the primary
+#, mirror; it is no longer modeled as a single blackbody, but instead is
+#, now modeled with one blackbody for each of the 18 primary mirror
+#, segments, with segment temperatures measured 1/2024.  The PM segments
+#, are assumed to have equal effective area x emissivity.
+#, 
+#, As in previous versions, the model approximates JWST with 15
+#, additional blackbodies representing major components.  What is new is
+#, that measured on-orbit temperatures are now used for components that
+#, have thermal sensors.  Of these 15 components, 9 have measured
+#, temperatures (PM frill, core, DTA tower, ISIM bench, TM FSM mask, AOS
+#, bench, secondary mirror, SM support structures,and BSF).  The other 6
+#, components do not have any temperature sensors (sunshield, sunshield
+#, spreaders, bib, AOS exterior, SS layer 4 leakage, and SS light line
+#, tolerance).
+#, 
+#, To fit the operational MIRI imager data, temperatures of components
+#, without measured temperatures were adjusted by hand, the frill was set
+#, 4K hotter than the measurements, and a small hot source (T~280K) was
+#, added to explain the short-wavelength MIRI data, while not
+#, over-predicting measurements from NIRCam at 4.4 micron.  This is by no
+#, means a unique fit, but represents the backgrounds seen in Cycles 1 and 2
+#, better than the current post-commissioning.  Work is ongoing to improve
+#, the measurement of the JWST thermal background. 
+#
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