PKS1424+240 (LST) analysis - neutrino candidate
Revision as of 09:41, 15 September 2024 by Gloria Maria Cicciari (talk | contribs) (→Analysis by Name (Institute - email))
Contents
- 1 General information
- 2 Analysis steps
- 3 Analysis information
- 4 Analysis results
- 4.1 Preliminary Theta2 plots
- 4.2 Inspect the DL3 file content
- 4.3 Plot temporal evolution of excess events and significance value
- 4.3.1 Examples of plots of counts+excess, exposure and energy migration of each selected dataset
- 4.3.2 Final spectral model
- 4.3.3 The LC Estimator on a run-by-run basis and nightly
- 4.3.4 Final Model
- 4.3.5 Light Curve (LC)
- 4.3.6 TS profile
- 4.3.7 Plot of residuals
- 4.3.8 Spectral Energy Distribution (SED)
General information
Name of the source: PKS 1424+240
Brief description of the source:
- It is the farthest BL Lac detected at TeV
- It is an IBL/HBL
- z ~ 0.6
- RA, Dec (deg) : 216.75163247, 23.80001042
Analysis by Name
- Davide Cerasole
- Gloria Maria Cicciari (gloriamaria.cicciari@unipa.it)
- Sara Fogliaceo
- Serena Loporchio
- Manuela Mallamaci
- Salvatore Mangano
- Giovanni Marsella
- Elisa Prandini
- Ilaria Viale
- Elisa Visentin
Data-taking information
Cycle I observations 2023-01-23 to 2023-07-17
- Dates of data-taking: 2023/01/23, 2023/01/27, 2023/03/10, 2023/04/18, 2023/05/12, 2023/05/15, 2023/05/22, 2023/07/17
- Observation runs selected are: [11805 11806 11807 11808 11933 11934 11935 11936 11937 12747 12748 12749 12750 12957 12958 12959 12960]
- Total livetime of all observations (hrs): 19.7
- Total livetime of selected observations (hrs): 4.5
- ZD range (deg): 0 - 60
Analysis steps
- R0 : uncalibrated RAW waveforms from the camera
- R1 : calibrated waveforms from the camera
- DL1a : integrated charge and peak position of the waveform
- DL1b : image parameters (width, length, intensity…)
- DL2 : event parameters (energy, direction, time…)
- DL3 : lists of reconstructed events after event selection with corresponding IRFs
Analysis information
Data quality
The list with the runs passing data quality
/fefs/aswg/data/real/DL1/20230123/v0.10/tailcut84/dl1_LST-1.Run11805.h5 /fefs/aswg/data/real/DL1/20230123/v0.10/tailcut84/dl1_LST-1.Run11806.h5 /fefs/aswg/data/real/DL1/20230123/v0.10/tailcut84/dl1_LST-1.Run11807.h5 /fefs/aswg/data/real/DL1/20230123/v0.10/tailcut84/dl1_LST-1.Run11808.h5 /fefs/aswg/data/real/DL1/20230128/v0.10/tailcut84/dl1_LST-1.Run11933.h5 /fefs/aswg/data/real/DL1/20230128/v0.10/tailcut84/dl1_LST-1.Run11934.h5 /fefs/aswg/data/real/DL1/20230128/v0.10/tailcut84/dl1_LST-1.Run11935.h5 /fefs/aswg/data/real/DL1/20230128/v0.10/tailcut84/dl1_LST-1.Run11936.h5 /fefs/aswg/data/real/DL1/20230128/v0.10/tailcut84/dl1_LST-1.Run11937.h5 /fefs/aswg/data/real/DL1/20230418/v0.10/tailcut84/dl1_LST-1.Run12747.h5 /fefs/aswg/data/real/DL1/20230418/v0.10/tailcut84/dl1_LST-1.Run12748.h5 /fefs/aswg/data/real/DL1/20230418/v0.10/tailcut84/dl1_LST-1.Run12749.h5 /fefs/aswg/data/real/DL1/20230418/v0.10/tailcut84/dl1_LST-1.Run12750.h5 /fefs/aswg/data/real/DL1/20230512/v0.10/tailcut84/dl1_LST-1.Run12957.h5 /fefs/aswg/data/real/DL1/20230512/v0.10/tailcut84/dl1_LST-1.Run12958.h5 /fefs/aswg/data/real/DL1/20230512/v0.10/tailcut84/dl1_LST-1.Run12959.h5 /fefs/aswg/data/real/DL1/20230512/v0.10/tailcut84/dl1_LST-1.Run12960.h5
Data storage
Monte Carlo simulations
/fefs/aswg/data/mc/DL2/AllSky 20240131_allsky_v0.10.5_all_dec_base/TestingDataset/dec_2276/
DL1 data
/fefs/aswg/data/real/DL1/YYYYMMDD/v0.10/tailcut84/dl1_LST-1.RunXXXXX.h5
Random forest
/fefs/aswg/data/models/AllSky/20240131_allsky_v0.10.5_all_dec_base/
DL2 data
/fefs/aswg/workspace/gloriamaria.cicciari/DL3/PKS1424/
DL3 data and IRF
/fefs/aswg/workspace/gloriamaria.cicciari/DL3/PKS1424/
Analysis results
Preliminary Theta2 plots
Theta2 plots obtained from DL2 data using the explore_DL2.ipynb code
Energy range: 0.0 - 0.2 TeV Excess: 690.000; Off: 155056 Gamma rate: 0.675 events / minute Off rate: 151.779 events / minute alpha (backg normalization): 1.000 Li & Ma Significance: 1.24 standard deviations
Energy range: 0.2 - 1000000.0 TeV Excess: -6.333; Off: 415 Gamma rate: -0.006 events / minute Off rate: 0.406 events / minute alpha (backg normalization): 0.333 Li & Ma Significance: 0.00 standard deviations
Inspect the DL3 file content
The used code is the post_DL3_analysis.ipynb
- Spatial distribution of events (typically on a plane of celestial coordinates such as RA/Dec or local altitude/azimuth coordinates)
- Energy distribution (spectrum of events)
- Temporal distribution (histogram of events over time)
- Angular offset distribution (angular distance from the centre of the field of view)
Selection of observations
Filters applied to select just a subset of the observation list based on source name, zenith angle or livetime
max_zen = 70 (in deg for a maximum limit on zenith pointing of observations) min_time = 300 (in seconds for minimum livetime of each observation)
Observation runs selected are: [11805 11806 11807 11808 11933 11934 11935 11936 11937 12747 12748 12749 12750 12957 12958 12959 12960] Total livetime of all observations: 19.7 h Total livetime of selected observations 4.5 hrs
Define Target position and energy ranges for reconstructed events
OrderedDict([('CREATOR', 'pyirf v0.10.1'),
('HDUDOC',
'https://github.com/open-gamma-ray-astro/gamma-astro-data-formats'),
('HDUVERS', '0.2'),
('HDUCLASS', 'GADF'),
('HDUCLAS1', 'RESPONSE'),
('HDUCLAS2', 'EFF_AREA'),
('HDUCLAS3', 'POINT-LIKE'),
('HDUCLAS4', 'AEFF_2D'),
('DATE', '2024-06-27 16:42:06.949'),
('TELESCOP', 'CTA-N'),
('INSTRUME', 'LST-1'),
('FOVALIGN', 'RADEC'),
('B_TOTAL', 38.592769622802734),
('B_INC', 0.6519277095794678),
('ZEN_PNT', 38.11381),
('AZ_PNT', 88.21244),
('B_DELTA', 60.12539),
('EXTNAME', 'EFFECTIVE AREA')])
Spectral Fit will be done in energy edges: [ 0.01584893 0.02511886 0.03981072 0.06309573 0.1 0.15848932 0.25118864 0.39810717 0.63095734 1 1.58489319 2.51188643 3.98107171 6.30957344 10] TeV LC will be estimated from 0.10000000000000002 TeV to 10.000000000000002 TeV
Data Reduction chain
safe_min_energy = 50 * u.GeV safe_max_energy = 20 * u.TeV
Spectrum Dataset for all observations
obs_id: 11805 obs_id: 11806 obs_id: 11807 obs_id: 11808 obs_id: 11933 obs_id: 11934 obs_id: 11935 obs_id: 11936 obs_id: 11937 obs_id: 12747 obs_id: 12748 obs_id: 12749 obs_id: 12750 obs_id: 12957 obs_id: 12958 obs_id: 12959 obs_id: 12960 CPU times: user 10min 31s, sys: 1min 4s, total: 11min 35s Wall time: 11min 41s
The target position and OFF regions used for the calculation of the excess
Theta2 plots
Theta2 plots obtained from DL3 data using the post_DL3_analysis.ipynb code
Excess plots
Excess plots obtained from DL3 data using the post_DL3_analysis.ipynb code
Plot temporal evolution of excess events and significance value
The following plots may indicate that there are problems with the observation (e.g. instrumental noise or incorrectly modelled background effects)
Examples of plots of counts+excess, exposure and energy migration of each selected dataset
Final spectral model
{'type': 'LogParabolaSpectralModel',
'parameters': [{'name': 'amplitude',
'value': 5e-12,
'unit': 'TeV-1 s-1 cm-2'},
{'name': 'reference', 'value': 0.5578072365055083, 'unit': 'TeV'},
{'name': 'alpha', 'value': 2.0},
{'name': 'beta', 'value': 0.1}]}
The LC Estimator on a run-by-run basis and nightly
{'name': 'amplitude',
'value': 4.7785201782428055e-12,
'unit': 'TeV-1 s-1 cm-2',
'error': 5.275533147495292e-12},
{'name': 'reference', 'value': 0.5578072365055083, 'unit': 'TeV'},
{'name': 'alpha', 'value': 2.8325177157861554, 'error': 4.102202154886328},
{'name': 'beta', 'value': 4.767544739308446, 'error': 12.26726001202649}
Final Model
{'name': 'PKS1424',
'type': 'SkyModel',
'spectral': {'type': 'LogParabolaSpectralModel',
'parameters': [{'name': 'amplitude',
'value': 4.7785201782428055e-12,
'unit': 'TeV-1 s-1 cm-2',
'error': 5.275533147495292e-12},
{'name': 'reference', 'value': 0.5578072365055083, 'unit': 'TeV'},
{'name': 'alpha', 'value': 2.8325177157861554, 'error': 4.102202154886328},
{'name': 'beta', 'value': 4.767544739308446, 'error': 12.26726001202649}]},
'FitResult': {'Optimize': OptimizeResult
backend : minuit
method : migrad
success : True
message : Optimization terminated successfully..
nfev : 152
total stat : 4.41
'Covariance': CovarianceResult
backend : minuit
method : hesse
success : True
message : Hesse terminated successfully.}}
Light Curve (LC)
The LC indicates that the flux in many observations is very low, as indicated by the upper limit arrows, which indicate that the source was not detected with certainty at those times. The error bars are quite large, suggesting considerable uncertainty in the flux measurements.
TS profile
This plot shows how the quality of the fit varies for different combinations of energy and differential flux. Specifically, the light region indicates where the model describes the data best, while the darker regions indicate where the fit is least consistent
Plot of residuals
Spectral Energy Distribution (SED)
The SED only returns upper limits (no significant quantity of photons were detected in this energy range, and therefore only an upper limit to the flux could be established)
The analysis will need to be fine-tuned because of the lack of detection
