Add script to fit NET vs. PWV

bolo-calc/pbdr_v2/fit_NET_v_pwv.py

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+import os
+import sys
+
+import matplotlib.pyplot as plt
+import numpy as np
+import toml
+
+
+table = toml.load("outputs_july27/NET_v_pwv.toml")
+
+pwv_ref = 1.0
+
+nrow, ncol = 2, 2
+fig = plt.figure(figsize=[12 * ncol, 6 * nrow])
+iplot = 0
+
+for key in table.keys():
+    if key.endswith(".yaml"):
+        subtable = table[key]
+        iplot += 1
+        ax = fig.add_subplot(nrow, ncol, iplot)
+        ax.set_title(key)
+        for band in subtable:
+            pwv = np.array(subtable[band]["pwv"]) * 1e-3
+            net = np.array(subtable[band]["NET"])
+            pivot_pwv = subtable[band]["xdefault"] * 1e-3
+            p = np.polyfit(pwv, net, 2)
+            pivot_net = np.polyval(p, pivot_pwv)
+            plt.plot(pwv, net / pivot_net, label=f"{band} : {pivot_net:.1f}", lw=3)
+            #plt.plot(np.log(pwv), np.log((net / pivot_net) ** 2), label=f"{band} : {pivot_net:.1f}", lw=3)
+            p /= pivot_net
+            x = np.linspace(0, 6, 100)
+            plt.plot(x, np.polyval(p, x), "k--", label=f"{band} : fit = {p[2]:.6f}, {p[1]:.6f}, {p[0]:.6f}")
+            #plt.plot(np.log(x), np.log(np.polyval(p, x) ** 2), "k--", label=f"{band} : fit = {p[2]:.6f}, {p[1]:.6f}, {p[0]:.6f}")
+            print(f"{key} {band} {p[2]:.6f}, {p[1]:.6f}, {p[0]:.6f}")
+        ax.set_ylim([0, 3])
+        ax.set_xlabel("PWV [mm]")
+        ax.set_ylabel("NET factor")
+        plt.legend(loc="best")
+fig.savefig("NET_v_pwv_fit.png")
+plt.show()

jbolo/2025/atmos

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+../atmos

jbolo/2025/yamls/Bicep3_90GHz.yaml

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+version: {date: 20250210, name: 'Bicep3_orig'}
+# Fixed LF wafer counts, which were off by a factor of two, and adjusted MF/HF for pixels lost to pins.
+# Setting spillovers to those calculated by P. Grimes here:
+# https://docs.google.com/spreadsheets/d/1dppe8RRixXaNPDD-mv_Fw45q-ndAt2ETHffZ9tGA1W0/edit?gid=439824212#gid=439824212
+#
+config:
+  dnu: 0.1 # GHz frequency resolution for integrals
+# We set dust and synchrotron very small so they are ignored.  Zero eventually throws an error.
+sources:
+  cmb: {source_type: blackbody, T: 2.726, emiss: 1.0}
+  # dust: {source_type: greybody, amplitude: 1e-5, scale_frequency: 353.0, scale_temperature: 19.7}
+  # synchrotron:  {source_type: powerlaw, spectral_index: -3.0, amplitude: 1e-10, scale_frequency: 30.0}
+  atmosphere:
+    # This shows how to do it with the bolo-calc hdf5 file.
+    source_type: hdf5  #
+    file: '../atmos/atm_20201217.hdf5'
+    site: 'Pole'
+    pwv: 321      # microns, from 0 to 8000.  321u for Pole from Kuo's paper, ~8 month observing season.
+    elevation: 55  # degrees, integer from 1 to 90
+optics_defaults: {temperature: 250.0, reflection: 0.0, scatter_frac: 0.0, spillover: 0.0, absorption: 0.0}
+optical_elements:
+  # requires python 3.7 or later, because we assume dict{} is ordered.
+  # This list of elements starts with the one closest to the sky, and moves toward the detector.
+  baffle:       {obj_type: Bespoke,    absorption: 0.0045}   # CV says 2021 paper value is not right, more like 3.3KRJ at 90GHz.
+    ##window:       {obj_type: LossTangent, reflection: 0.003, thickness: 0.010, index: 1.525, loss_tangent: 2.22E-4}
+  window:       {obj_type: LossTangent, temperature: 260.0,reflection: 0.003, thickness: 0.03175, index: 1.525, loss_tangent: 2.22E-4}
+  RTMLI_10 :    {obj_type: Bespoke,     temperature: 150.0,absorption: [0.006, 0.006] }  # 10 layers
+  hwp:          {obj_type: Bespoke,     temperature: 1.0,  absorption: [0.00001, 0.00001] }
+  alumina_filt: {obj_type: LossTangent, temperature: 50.0, reflection: 0.02, thickness: 0.010, index: 3.1, loss_tangent: 3.0E-4}
+  lyot:         {obj_type: Bespoke,     temperature: 5.5,  absorption: [0.13, 0.06]}   # 0.13 is from Bicep3 paper
+  lens1:        {obj_type: LossTangent, temperature: 5.5,  reflection: 0.02, thickness: 0.021, index: 3.1, loss_tangent: 3.0E-4}
+  nylon_filt:   {obj_type: Bespoke,     temperature: 5.5,  reflection: 0.01, absorption: [0.006,  0.025]}
+  lens2:        {obj_type: LossTangent, temperature: 5.5,  reflection: 0.02, thickness: 0.027, index: 3.1, loss_tangent: 3.0E-4} 
+  lowpass:      {obj_type: Bespoke,     temperature: 5.0,  absorption: 0.01, reflection: 0.05}
+bolo_config:
+  # For aperture stop calcs
+  waist_factor: 3.0
+  f_number: 1.45  #
+  #
+  N_polarizations: 1
+  #
+  AOmega_method: ModeCount   # or "Fixed"
+  N_modes: 1  # required if method == "ModeCount"
+  #
+  # # options:  "from_optical_power", in which case psat = P_optical * psat_factor,
+  # or "specified", in which case it is given for each detector channel explicitly.
+  psat_method: 'from_optical_power'
+  psat_factor: 2.5  # must a number if psat_method is "from_optical_power"
+  beta: 2.5   # (from arXiv:1403.4302 for Bicep3, n=2.5) this is beta = n-1. bolo-calc called it "carrier index". Note that G_dynamic is found from psat, T_c, and carrier_index
+  #
+  T_bath: 0.268
+  T_c: 0.48
+  R_bolo: 0.08   # as biased in operation, ie less than R_normal
+  yield: 0.8
+  num_wafers_per_tube: 12
+  optically_good_det_fraction: 1.0
+readout:
+#  method: 'fraction'  #in anticipation of getting NEI number/formula.
+  method: 'from_NEI'   # uses channels readout_NEI
+channels:
+  MF_1:
+    chnum: 0  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  96.1  # not used
+    # Based on quoted bandwidth in paper
+    nu_low: 82.5        # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 109.9
+    #
+    # Based on H.Hui's email saying he used 25% bandwidth
+    #nu_low: 84.09        
+    #nu_high: 108.11
+    #
+    #read_frac: 0.05
+    readout_NEI: 12.0e-12 # A/rtHz, see fig 21 of arXiv:2110.00482, then multiply by sqrt(2) to get from uArtsec to uA/rtHz.
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.480 
+    #psat: 4.60e-12  # see psat_method above.
+    horn_diameter: 7.5e-3   # square patch size from Bicep3 paper.
+    pixel_spacing: 8.0e-3
+    num_det_per_wafer: 100    # 9/24/2024, 215 actual pixels (217-2 for pins), 430 detectors/band
+  MF_2:
+    chnum: 1  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  150.0  # not used
+    nu_low: 131.25       # centered at 150GHz, 25% fractional bandwidth.
+    nu_high: 168.75
+    #read_frac: 0.05
+    readout_NEI: 8.0e-12 # A/rtHz, see fig 21 of arXiv:2110.00482
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.50
+    #psat: 4.60e-12  # see psat_method above.
+    horn_diameter: 7.5e-3   # meters
+    pixel_spacing: 8.0e-3
+    num_det_per_wafer: 100   # 9/24/2024, 215 actual pixels (217-2 for pins), 430 detectors/band

jbolo/2025/yamls/SAT_HWP_aggr_20241121_phase2.yaml

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+version: {date: 20241121, name: 'S4_aggr+HWP_phase2'}
+# Fixed LF wafer counts, which were off by a factor of two, and adjusted MF/HF for pixels lost to pins.
+# Setting spillovers to those calculated by P. Grimes here:
+# https://docs.google.com/spreadsheets/d/1dppe8RRixXaNPDD-mv_Fw45q-ndAt2ETHffZ9tGA1W0/edit?gid=439824212#gid=439824212
+#
+config:
+  dnu: 0.1 # GHz frequency resolution for integrals
+# We set dust and synchrotron very small so they are ignored.  Zero eventually throws an error.
+sources:
+  cmb: {source_type: blackbody, T: 2.726, emiss: 1.0}
+  # dust: {source_type: greybody, amplitude: 1e-5, scale_frequency: 353.0, scale_temperature: 19.7}
+  # synchrotron:  {source_type: powerlaw, spectral_index: -3.0, amplitude: 1e-10, scale_frequency: 30.0}
+  atmosphere:
+    # This shows how to do it with the bolo-calc hdf5 file.
+    source_type: hdf5  #
+    file: '../atmos/atm_20201217.hdf5'
+    site: 'Atacama'
+    pwv: 993      # microns, from 0 to 8000.  321u for Pole from Kuo's paper, ~8 month observing season.
+    elevation: 50  # degrees, integer from 1 to 90
+optics_defaults: {temperature: 273.0, reflection: 0.0, scatter_frac: 0.0, spillover: 0.0, absorption: 0.0}
+optical_elements:
+  # requires python 3.7 or later, because we assume dict{} is ordered.
+  # This list of elements starts with the one closest to the sky, and moves toward the detector.
+  baffle:       {obj_type: Bespoke,    absorption: 0.01}
+  window:       {obj_type: LossTangent, reflection: 0.003, thickness: 0.020, index: 1.525, loss_tangent: 3.0E-4}
+  RTMLI_10 :    {obj_type: Bespoke,     temperature: 150.0, absorption: [0.00399, 0.00399, 0.00399, 0.00399, 0.00399, 0.00399, 0.00435, 0.0083] }  # 10 layers
+  hwp:          {obj_type: LossTangent, temperature: 55.0, reflection: 0.02, thickness: 0.004, index: 3.1, loss_tangent: 3.0E-4}
+  alumina_filt: {obj_type: LossTangent, temperature: 50.0, reflection: 0.02, thickness: 0.010, index: 3.1, loss_tangent: 3.0E-4}
+  nylon_filt:   {obj_type: Bespoke,     temperature:  4.0, reflection: 0.01, absorption: [0.0003, 0.0007, 0.0056, 0.0075, 0.0223, 0.0265, 0.0698, 0.123 ]}
+  lens1:        {obj_type: LossTangent, temperature: 1.0,  reflection: 0.02, thickness: 0.055, index: 1.52, loss_tangent: 1.0E-4}
+  # lyot abs numbers from Grimes: 
+  # https://docs.google.com/spreadsheets/d/1dppe8RRixXaNPDD-mv_Fw45q-ndAt2ETHffZ9tGA1W0/edit?gid=439824212#gid=439824212
+  lyot:         {obj_type: Bespoke,     temperature: 1.0,  absorption: [0.482, 0.227, 0.512, 0.458, 0.160, 0.127, 0.06, 0.02]}  
+  lens2:        {obj_type: LossTangent, temperature: 1.0,  reflection: 0.02, thickness: 0.059, index: 1.52, loss_tangent: 1.0E-4} 
+  lowpass:      {obj_type: Bespoke,     temperature: 0.1,  absorption: 0.01, reflection: 0.05}
+bolo_config:
+  # For aperture stop calcs
+  waist_factor: 3.0
+  f_number: 1.45  #
+  #
+  N_polarizations: 1
+  #
+  AOmega_method: ModeCount   # or "Fixed"
+  N_modes: 1  # required if method == "ModeCount"
+  #
+  # # options:  "from_optical_power", in which case psat = P_optical * psat_factor,
+  # or "specified", in which case it is given for each detector channel explicitly.
+  psat_method: 'from_optical_power'
+  psat_factor: 2.5  # must a number if psat_method is "from_optical_power"
+  beta: 2.7   # this is beta = n-1. bolo-calc called it "carrier index". Note that G_dynamic is found from psat, T_c, and carrier_index
+  #
+  T_bath: 0.1
+  T_c: 0.16
+  R_bolo: 0.006   # as biased in operation, ie less than R_normal
+  yield: 0.8
+  num_wafers_per_tube: 12
+  optically_good_det_fraction: 1.0
+readout:
+#  method: 'fraction'  #in anticipation of getting NEI number/formula.
+  method: 'from_NEI'   # uses channels readout_NEI
+channels:
+  LF_1:
+    chnum: 0  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  24.75  # not used
+    nu_low: 21.50        # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 28.00
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 1.0e-12  # see psat_method above.
+    horn_diameter: 18.95e-3   # meters
+    pixel_spacing: 19.1e-3
+    num_det_per_wafer: 74  #9/24/2024, 19 pixels/wafer
+  LF_2:
+    chnum: 1  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  36.5  # not used
+    nu_low: 28.0        # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 45.0
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 4.18e-12  # see psat_method above.
+    horn_diameter: 18.95e-3   # meters
+    pixel_spacing: 19.1e-3
+    num_det_per_wafer: 74  #9/24/2024, 19 pixels/wafer
+  MF_1_1:
+    chnum: 2  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  85.0  # not used
+    nu_low: 74.8        # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 95.2
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 4.60e-12  # see psat_method above.
+    horn_diameter: 5.15e-3   # meters
+    pixel_spacing: 5.3e-3
+    num_det_per_wafer: 860   # 9/24/2024, 215 actual pixels (217-2 for pins), 430 detectors/band
+  MF_2_1:
+    chnum: 3  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  95.0  # not used
+    nu_low: 83.6        # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 106.4
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 12.51e-12  # see psat_method above.
+    horn_diameter: 5.15e-3   # meters
+    pixel_spacing: 5.30e-3
+    num_det_per_wafer: 860   # 9/24/2024, 269 actual pixels, (271-2 for pins), so 538
+  MF_1_2:
+    chnum: 4  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  145.0  # not used
+    nu_low: 129.05       # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 160.95
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 4.60e-12  # see psat_method above.
+    horn_diameter: 5.15e-3   # meters
+    pixel_spacing: 5.3e-3
+    num_det_per_wafer: 860   # 9/24/2024, 215 actual pixels (217-2 for pins), 430 detectors/band
+  MF_2_2:
+    chnum: 5  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  155.0  # not used
+    nu_low: 137.95       # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 172.05
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 4.60e-12  # see psat_method above.
+    horn_diameter: 5.15e-3   # meters
+    pixel_spacing: 5.3e-3
+    num_det_per_wafer: 860 # 9/24/2024, 269 actual pixels, (271-2 for pins), so 538
+  HF_1:
+    chnum: 6  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  227.0  # not used
+    nu_low: 198.0        # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 256.0
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 1.0e-12  # see psat_method above.
+    horn_diameter: 5.05e-3   # meters
+    pixel_spacing: 5.2e-3
+    num_det_per_wafer: 934
+  HF_2:
+    chnum: 7  # This sets the order of lists in optical elements, must start at zero and increment from there.
+    band_center:  285.5  # not used
+    nu_low: 256.0       # if a band_response file is given, these set the low and high limits of integration.
+    nu_high: 315.0
+    #read_frac: 0.05
+    readout_NEI: 45.0e-12 # A/rtHz
+    band_response : {method: flat}
+    #band_response : {method: bandfile, fname : spt3g_90_pixelband.txt }
+    det_eff: 0.65
+    #psat: 4.18e-12  # see psat_method above.
+    horn_diameter: 5.05e-3   # meters
+    pixel_spacing: 5.2e-3
+    num_det_per_wafer: 934