Light and clarity in KM3NeT Jordan Seneca My goal for this - - PowerPoint PPT Presentation

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Light and clarity in KM3NeT Jordan Seneca My goal for this - - PowerPoint PPT Presentation

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Light and clarity in KM3NeT Jordan Seneca My goal for this presentation Inspire, stimulate questions and discussion 05/23/19 Jordan Seneca 2 Working towards a better ARCA res What I find exciting about my work How to convey

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Light and clarity in KM3NeT

Jordan Seneca

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My goal for this presentation

Inspire, stimulate questions and discussion

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 Working towards a better ARCA res  What I find exciting about my work  How to convey excitement to others

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 Working towards a better ARCA res  What I find exciting about my work  How to convey excitement to others

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Last year, in Dalfsen

Me

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Current reconstruction Aanet PDFs

PMT position 1 PMT direction Reception angle

New reconstruction Jpp PDFs

PMT position 2 PMT directions Reception angle Arrival time

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I found weird stuff.

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I found bugs in Jpp PDFs.

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I found bugs in Jpp PDFs.

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Bugs have now been fixed!

Thank you Maarten MC truth New reco Old reco

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Bugs have now been fixed!

Thank you Maarten

Sub 1 deg resolution

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Bugs have now been fixed!

Thank you Maarten

Sub 1 deg resolution

Not t so

  • fa

fast !!! !!!

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 Working towards a better ARCA res  What I find exciting about my work  How to convey excitement to others

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 Why are Jpp and AAnet PDFs

different?

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disagreement Jpp PDF: based on theoretical approximations AAnet PDF: MC interpolation

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 Why are Jpp and AAnet PDFs

different?

 N-scattered light? Other

approximations?

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When close, a lot of direct light

25m, PMT angle -1.0

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When far away, mostly 1- scattered light

100m, PMT angle -1.0

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When very far away, only 1- scattered light?

400m, PMT angle -1.0

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 Why are Jpp and AAnet PDFs

different?

 N-scattered light? There are other

approximations we could try.

 Re-emission?

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Less than 60% of visible light is not absorbed after 100m 63% 0.1%

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Less than 60% of the light is not absorbed after 100m 63% 0.1% All these hard photons are absorbed. Re-emission in visible?

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 Why are Jpp and AAnet PDFs

different?

 N-scattered light? There are other

approximations we could try.

 Re-emission?  Spread of particle shower

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63% 0.1% At low energies, showers are small

Particle shower Cherenkov photons

Not so much at high energies How does the longitudinal and radial spread affect the light profile?

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*dis *distant nt sni nicke ker*

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 Working towards a better ARCA res  What I find exciting about my work  How to convey excitement to others

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Exhibit A: The type of slides we show each

  • ther during collaboration meetings

in KM3NeT

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Analysis Visibility DATA Progress status Conclusion ATel BACKUP Sensitivities

Astronomy Telegram : 17-01-2018 announcements

11184 FACT : Exceptional Flare of Mrk 421 at TeV energies

Since December 2017, Mrk 421 has been showing already some activity at TeV energies, as reported in the ATels #11077 and #11086 by the FACT and HAWC collaborations. The source was observed by FACT for a total of 5.5 hours between 1:15 UTC and 7:05 UTC (MJD 58135). At the beginning of the observation, the source showed a flux of about 6-7 times that

  • f the Crab Nebula (CU) at TeV energies, then increasing to more than 9 CU. Over the whole
  • bservation, the flux was varying between 3 and 10 CU with a decrease towards the end of

the night and an average flux of roughly 6 CU.

11186 MAXI/GSC : detection of a rapid X-ray brightening from Mrk 421 11194 HAWC : observation of Mrk421 reaching peak TeV flux in month-long enhanced activity

( 6 equivalent CU) between 2018-01-17 06:39 and 09:47 UTC. This is about 10 times the all-time averaged flux measured by HAWC and the highest one since the beginning of this enhanced period. Enhanced emission has also been reported by FACT (ATel #11086 and #11184), and MAXI/GSC (ATel #11186).

11195 Swift/BAT : finds hard X-Ray flaring activity correlated with an

  • ngoing TeV flare of Mrk421

11199 TACTIC : detection of a strong TeV flare from Mrk 421

Multi-wavelength observations of this enhanced activity of the source have also been reported by FACT ( ATels : #11184), HAWC ( ATel : #11194), MAXI/GSC ( ATel : #11186) & Swift/BAT ( ATel : #11195). An exceptional flare was reported by FACT at TeV energies between 1:15 UTC and 7:05 UTC on Jan 17 (MJD 58135) with a maximum of >10 CU and a decrease towards the end of the night. The ongoing flaring activity of Mrk421 at TeV energies was already reported since December 2017 by the FACT and HAWC collaboration (ATels #11077 and #11086).

Mukharbek Organokov Université de Strasbourg HAWC blazars analysis 25 October 2018 22 / 28

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Why?

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 “I need to know what to say”

 Use notes in your

PowerPoint-like program

 Do a dry run

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 “I need to know what to say”  “Slides are used as work logs”

There are other ways of logging work:

 Elog  Wiki  Uploading .ppt with notes  Uploading .pdf with notes  Backup slides

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 “I need to know what to say”  “Slides are used as work logs”  “It takes effort to make nice slides”

The KM3NeT template will help with that

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The KM3NeT template

 Slide types  Predetermined fonts  Predetermined colors  Bank of logos  Bank of images

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Search for

Neutrino counterparts

  • f HAWC point-sources

Michael Smith Margaret Davis

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 PMT efficiency calibration update  K40 simulations comparison  K40 simulation updates

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Data/MC comparison

Variables: tcosth > 0 (upgoing), λ >-5.6 -5.4 -5.2 -5.0 -4.8 (AAFit) or χ2 <0.9 0.8 0.7 0.6 (BBFit) estimate of angular error β < 1◦ (AAFit) With previous best cut 6466 tracks (2007-16), 5862 tracks (2007-15), 678 tracks (2017). Still processing mupage ntuples 2017 only 2007-17

3 / 12

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Data/MC comparison

Variables: tcosth>0 (upgoing), λ > -5.6 -5.4 -5.2 -5.0 -4.8 (AAFit) or χ 2 <0.9 0.8 0.7 0.6 (BBFit) estimate of angular error β < 1 ◦ (AAFit) With previous best cut 6466 tracks (2007-16), 5862 tracks (2007-15), 678 tracks (2017). Still processing mupage ntuples

2017 only 2007 - 17

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Data/MC comparison

Variables: tcosth>0 (upgoing), λ > -5.6 -5.4 -5.2 -5.0 -4.8 (AAFit) or χ 2 <0.9 0.8 0.7 0.6 (BBFit) estimate of angular error β < 1 ◦ (AAFit) With previous best cut 6466 tracks (2007-16), 5862 tracks (2007-15), 678 tracks (2017). Still processing mupage ntuples

2017 only 2007 - 17

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Data/MC comparison

Variables: tcosth>0 (upgoing), λ > -5.6 -5.4 -5.2 -5.0 -4.8 (AAFit) or χ 2 <0.9 0.8 0.7 0.6 (BBFit) estimate of angular error β < 1 ◦ (AAFit) With previous best cut 6466 tracks (2007-16), 5862 tracks (2007-15), 678 tracks (2017). Still processing mupage ntuples

2017 only 2007 - 17

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Data/MC comparison

Looking at upgoing neutrinos from GC With previous best cut 6466 tracks (2007-16), 5862 tracks (2007-15), 678 tracks (2017). Still processing mupage ntuples

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Data/MC comparison

Looking at upgoing neutrinos from GC 2007 - 17: 7.2k tracks 2017: 0.7k tracks Muons not included in MC Is there an excess?

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Data/MC comparison

Looking at upgoing neutrinos from GC 2007 - 17: 7.2k tracks 2017: 0.7k tracks Muons not included Is there an excess?

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Data/MC comparison

Looking at upgoing neutrinos from GC 2007 - 17: 7.2k tracks 2017: 0.7k tracks Muons not included in MC Is there an excess?

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Data/MC comparison

Variables: tcosth > 0 (upgoing), λ >-5.6 -5.4 -5.2 -5.0 -4.8 (AAFit) or χ2 <0.9 0.8 0.7 0.6 (BBFit) estimate of angular error β < 1◦ (AAFit) With previous best cut 6466 tracks (2007-16), 5862 tracks (2007-15), 678 tracks (2017). Still processing mupage ntuples 2017 only 2007-17

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“Looks good enough to be used out

  • f the box,

is simple enough that it will rarely need cleaning up.”

~ me

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I am working towards improving the reconstruction of showers in ARCA Light in our detector is interesting and important to think about The KM3NeT template is in the works for streamlining quality presentations