Research presentation2015

AGN Feedback Study in Young QuasarsAn Ongoing search for Young Jets

December 15, 2015

Poon [email protected]

mailto:[email protected]

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ASTRO9995 ResearchPresentation

Poon Panichpibool

AGN Project OverviewBackground of the Project

Background of the Project

Research Groups

Optical Part of ProjectUVa OHSU WISE project

LBT Observation

WISE project at UVaResearch Group at UVa

Current Goals

Data Reduction by IRAF

Astrometric Calibration andCoadding

Photometric Calibration

Future PlanPlan for Winter 2015 andSpring 2016

Q&AQuestion?

Contact Information

Agenda

AGN Project OverviewBackground of the ProjectBackground of the ProjectResearch Groups

Optical Part of ProjectUVa OHSU WISE projectLBT Observation

WISE project at UVaResearch Group at UVaCurrent GoalsData Reduction by IRAFAstrometric Calibration and CoaddingPhotometric Calibration

Future PlanPlan for Winter 2015 and Spring 2016

Q&AQuestion?Contact Information

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Poon Panichpibool

AGN Project Overview2 Background of the Project


Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Why study AGN?I The active galactic nucleus (AGN) which is driven by

accretion onto supermassive black holes, is an importantkey to understand the evolution of the universe.

I AGNs effectively influence the formation and subsequentevolution of galaxies and resident stars, gas and dust.

I The origin of the AGN phenomenon is started ingravitational interactions on galactic scales, with accretionmaterials in the form of gas and dust into galactic nuclei.

I But the details of the process are mostly heavily obscuredfrom view by gaseous and dusty region, especially forAGNs which recently triggered by merger activities.

I This compact (sub-arcsecond) obscured nuclear region is,however, transparent and therefore directly observable atradio wavelengths.

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Poon Panichpibool


3 Background of the Project

Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Why study Young Jets from AGN?I Massive Black Hole in AGN affect the galaxy mass

through feedback.I Mass Accretion from AGN’s Black Hole result in negative

feedback i.e. expel ISM material away, slowing theaccretion. Hence, star formations is quenched.

I But the details of the process are mostly heavily obscuredfrom view by gaseous and dusty region, especially forAGNs which recently triggered by merger activities.

I Quasar mode feedback observed in AGN with Eddintonlimited luminosity.

I The Quasar winds blow the ISM gaseous material away.I Want to study the effect of powerful AGN jets on the ISM.I Want to be able to see the early interaction between the

Jets and ISM i.e. trying to catch the early phase of the Jet!where the ISM has not yet blown away.

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Poon Panichpibool



4 Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information

AGN Project OverviewResearch Group

There are two research groups for this project.I Optical part research group which focus on optical data

from UVa OHSU WISE project.I Radio Astronomy part research group which focus on

Radio data this group consists of Dr. Carol Lonsdale, Dr.Mark Lacy at NRAO, Pallavi Patil and Adam Trap.

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Poon Panichpibool



Research Groups

Optical Part of Project5 UVa OHSU WISE project

LBT Observation


Current Goals





Q&AQuestion?

Contact Information


I This non-radio astronomy research is a collaborationbetween UVa astronomy and OHSU astronomy which Dr.Mark Whittle is a Principal Investigator.

I Focus on rate samples of distant (1.4 < z < 3) heavilyobscured and extremely luminous quasars with youngradio jets.

I Targets have been selected from the WISE mid-infrared(MIR) survey cross-matched with the NRAO VLA SkySurvey (NVSS).

I We retrieve our data from the Large Binocular Telescope(LBT) using LBC cameras.

I LBT observation started in January 2014 to April 2015with 17 Different Objects.

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Poon Panichpibool



Research Groups


6 LBT Observation


Current Goals





Q&AQuestion?

Contact Information

Optical Part of ProjectLBT Observation

I The Large Binocular Telescope or LBT is an opticaltelescope for astronomy located on Mount Graham(10,700-foot (3,300 m)) in the Pinaleno Mountains ofsoutheastern Arizona.

I The LBT is currently one of the world’s most advancedoptical telescopes; using two 8.4 m (27 ft) wide mirrors,with a 14.4 m center-center separation, it has the samelight gathering ability as an 11.8 m (39 ft) wide singlecircular telescope and detail of a 22.8 m (75 ft) wide one.

I LBT has several instruments that we can use forastronomy research such as LBC, PEPSI, MODS, LUCI,LINC/Nirvana, ARGOS.

I We use the Large Binocular Camera LBC for ourobservation.

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Poon Panichpibool



Research Groups


7 LBT Observation


Current Goals





Q&AQuestion?

Contact Information

Optical Part of ProjectLBC

I The LBC are two wide-field cameras that are mounted onthe prime focus swing arms of the LBT.

I The LBC Blue is mounted above the left (SX) mirror and isblue-optimized for observations from approximately 3500to 6500 angstroms.

I The LBC Red is mounted above the right (DX) mirror andis red-optimized for observations from approximately 5500angstroms to 1 micron.

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Poon Panichpibool



Research Groups


8 LBT Observation


Current Goals





Q&AQuestion?

Contact Information

Optical Part of ProjectLBC

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Poon Panichpibool



Research Groups


LBT Observation

WISE project at UVa9 Research Group at UVa

Current Goals





Q&AQuestion?

Contact Information

WISE project at UVaResearch Group

Researchers in WISE project at UVaI Dr. Mark WhittleI Dr. Ricky PattersonI Poon Panichpibool

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Poon Panichpibool



Research Groups


LBT Observation


10 Current Goals





Q&AQuestion?

Contact Information

WISE project at UVaCurrent Goals

Current GoalsI Finish combining all object frames to be used in further

analysis. The coordinate of objects in the field should bequite precise to be able to compare with Radio result.

I Finish photometric Calibration for all objects using SDSSas a main calibration. If objects are not in the SDSS’ footprint, then have to do some conversion between othercatalogs and SDSS.

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals

11 Data Reduction by IRAF




Q&AQuestion?

Contact Information

WISE project at UVaData Reduction by IRAF

LBC data ReductionI There is no main pipeline for reducing LBC data.I However, there are several methods to reduce LBC data.

1. LBC_redux package by Dr. Neil Crightonhttps://github.com/nhmc/LBC_redux

2. LBC GUI pipeline V 1.0 (DEC2007) by INAF AstronomicalObservatory of Romehttp://lbc.oa-roma.inaf.it/commissioning/data/LBCGUI_PIPELINE/index.html#intro

3. LBC-reduction package by Dr. Benjamin Weinerhttps://github.com/bjweiner/LBC-reduction

I These Methods are not easy to use. We decide to haveour own pipeline for UVa Astronomy.https://github.com/poonpa/lbc

I We use IRAF CCDRED package to reduce our data. Thenwe follow our pipeline for Astrometric Calibration andCoadding.

https://github.com/nhmc/LBC_redux

http://lbc.oa-roma.inaf.it/commissioning/data/LBCGUI_PIPELINE/index.html#intro

http://lbc.oa-roma.inaf.it/commissioning/data/LBCGUI_PIPELINE/index.html#intro

https://github.com/bjweiner/LBC-reduction

https://github.com/poonpa/lbc

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals


12 Astrometric Calibration andCoadding



Q&AQuestion?

Contact Information

WISE project at UVaAstrometric Calibration and Coadding

Astrometric Calibration by SCAMP and SWARP1

I By combining images using Imcombine task in IRAF, itturn out that objects’WCS coordinates are not aligned withCatalog’s coordinate in DS9.

1SCAMP and SWARP by Dr. Emmanuel Bertin

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Astrometric Calibration by SCAMP and SWARPI We decide to use SExtractor, SCAMP and SWARP2 to fix

any astrometic problem and coadding objects frames.Here are stepsSExtractor⇒ Retrieve catalog from all object frames↓SCAMP⇒ use Retrieved catalogs and Reference catalogto get Astrometic corrrection, stored in new header foreach object frame.↓SWARP⇒ use corrected header to "Swarp" each objectframe in order to achieve correct coordinates, then stackand combine all object frames.↓Now you have an astrometry corrected combined objectframes ready to be used!

2Programs by Dr. Emmanuel Bertin

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Figure: Zoom in of Astrometric Calibrated and Coadded Image. Thepink circles are SDSS R-6’s Catalog overlay.

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals



16 Photometric Calibration


Q&AQuestion?

Contact Information

WISE project at UVaPhotometric Calibration

Photometric CalibrationI Once we obtain an astrometric calibrated images, we have

to perform a photometric calibration.I The Photometric Calibration will allow us to understand

the Magnitude of objects i.e. derive the Magnitudeconversion equation which will convert Object’s counts inADU to SDSS’s r-Magnitude and g-Magnitude.

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Photometric CalibrationI For objects in the SDSS database, photometric calibration

is performed in following steps1. Retrieving photometric data from SDSS including PSF

magnitude and Error of PSF Magnitude.2. Cross Matching data tables from SDSS database and

SExtractor’s master catalog.3

3. Selecting only non-saturated stars to work on calibrationusing SExtractor’s parameters.

4. Converting SDSS’s Asinh Magnitude to Pogson Magnitudebefore running the calibration.

5. Running the Calibration using IDL program.

3There are several methods to do but currently I use my own IDL program toperform cross matching which is still not optimized.

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Photometric CalibrationReasoning for using Pogson Magnitude instead of SDSS’sAsinh Magnitude.

I SDSS’s Asinh Magnitude was created to eliminate problemwith negative counts which is a problem in Pogson system.

I Here is the SDSS Asinh Magnitude equation4:

Mag = −(2.5/ln(10)) ∗ [asinh((f/fo)/2b) + ln(b)] (1)

fo = 10aa+kk∗Airmass5 (2)

I Problem arise with Softening Parameter "b" and fo i.e.What’s fo for our data?

I Plot between SDSS’Asinh versus SExtractor’s PSFmagnitude show some non linearity.

4Lupton et al. 19995aa=Zero point, kk=Extinction Coefficient from Bouguer’s Law

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information


Figure: Photometric Calibration Plot of SDSS’s PSF Magnitude VersusObjects’Asinh Magnitude.

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information



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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information



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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

Contact Information



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Poon Panichpibool



Research Groups


LBT Observation


Current Goals




Future Plan23 Plan for Winter 2015 and

Spring 2016

Q&AQuestion?

Contact Information

Future PlanWhat’s Next?

Here are tentative goals for the Winter break and nextsemester.

1. Finish Photometric Calibration for Objects in Non-SDSSfields i.e. using different Catalog to perform calibration.

2. Finish Writing a manual for LBC data reduction,Astrometric calibration and photometric calibration6. Thisguide will serve as a comprehensive manual for anyone atthe Astronomy Department to be able to reduce data fromthe LBT archive.

3. Further study the physical properties of WISE objects asthe current reduced data allow.

6I have already create a Github page to store all required files and manual.

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&A24 Question?

Contact Information

Q&AQuestions Time

If you have any question, please feel free to ask me.Credit to sharelatex website. 7

7This presentation is created by LATEX

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Poon Panichpibool



Research Groups


LBT Observation


Current Goals





Q&AQuestion?

25 Contact Information

Q&AContact Information

In case you have any comments, suggestions or have foundadditional information, please do not hesitate to contact me.You can find my contact details below.

Poon [email protected]

2021 Ivy Road, Apt. B4Charlottesville, VA 22903

mailto:[email protected]

Thank you for your attention!

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Research presentation2015