Research Presentation

1. AGN Feedback Study in Young Quasars
An Ongoing search for Young Jets
December 15, 2015
Poon Panichpibool
pp9mx@virginia.edu

2. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
Agenda
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and Spring 2016
Q&A
Question?
Contact Information

3. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
2 Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
AGN Project Overview
Background of the Project
Why study AGN?
The active galactic nucleus (AGN) which is driven by
accretion onto supermassive black holes, is an important
key to understand the evolution of the universe.
AGNs effectively influence the formation and subsequent
evolution of galaxies and resident stars, gas and dust.
The origin of the AGN phenomenon is started in
gravitational interactions on galactic scales, with accretion
materials in the form of gas and dust into galactic nuclei.
But the details of the process are mostly heavily obscured
from view by gaseous and dusty region, especially for
AGNs which recently triggered by merger activities.
This compact (sub-arcsecond) obscured nuclear region is,
however, transparent and therefore directly observable at
radio wavelengths.

4. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
3 Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
AGN Project Overview
Background of the Project
Why study Young Jets from AGN?
Massive Black Hole in AGN affect the galaxy mass
through feedback.
Mass Accretion from AGN’s Black Hole result in negative
feedback i.e. expel ISM material away, slowing the
accretion. Hence, star formations is quenched.
But the details of the process are mostly heavily obscured
from view by gaseous and dusty region, especially for
AGNs which recently triggered by merger activities.
Quasar mode feedback observed in AGN with Eddinton
limited luminosity.
The Quasar winds blow the ISM gaseous material away.
Want to study the effect of powerful AGN jets on the ISM.
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.

5. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
4 Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
AGN Project Overview
Research Group
There are two research groups for this project.
Optical part research group which focus on optical data
from UVa OHSU WISE project.
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.

6. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
5 UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
Optical Part of Project
UVa OHSU WISE project
This non-radio astronomy research is a collaboration
between UVa astronomy and OHSU astronomy which Dr.
Mark Whittle is a Principal Investigator.
Focus on rate samples of distant (1.4 < z < 3) heavily
obscured and extremely luminous quasars with young
radio jets.
Targets have been selected from the WISE mid-infrared
(MIR) survey cross-matched with the NRAO VLA Sky
Survey (NVSS).
We retrieve our data from the Large Binocular Telescope
(LBT) using LBC cameras.
LBT observation started in January 2014 to April 2015
with 17 Different Objects.

7. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
6 LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
Optical Part of Project
LBT Observation
The Large Binocular Telescope or LBT is an optical
telescope for astronomy located on Mount Graham
(10,700-foot (3,300 m)) in the Pinaleno Mountains of
southeastern Arizona.
The LBT is currently one of the world’s most advanced
optical telescopes; using two 8.4 m (27 ft) wide mirrors,
with a 14.4 m center-center separation, it has the same
light gathering ability as an 11.8 m (39 ft) wide single
circular telescope and detail of a 22.8 m (75 ft) wide one.
LBT has several instruments that we can use for
astronomy research such as LBC, PEPSI, MODS, LUCI,
LINC/Nirvana, ARGOS.
We use the Large Binocular Camera LBC for our
observation.

8. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
7 LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
Optical Part of Project
LBC
The LBC are two wide-field cameras that are mounted on
the prime focus swing arms of the LBT.
The LBC Blue is mounted above the left (SX) mirror and is
blue-optimized for observations from approximately 3500
to 6500 angstroms.
The LBC Red is mounted above the right (DX) mirror and
is red-optimized for observations from approximately 5500
angstroms to 1 micron.

9. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
8 LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
Optical Part of Project
LBC

10. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
9 Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Research Group
Researchers in WISE project at UVa
Dr. Mark Whittle
Dr. Ricky Patterson
Poon Panichpibool

11. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
10 Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Current Goals
Current Goals
Finish combining all object frames to be used in further
analysis. The coordinate of objects in the field should be
quite precise to be able to compare with Radio result.
Finish photometric Calibration for all objects using SDSS
as a main calibration. If objects are not in the SDSS’ foot
print, then have to do some conversion between other
catalogs and SDSS.

12. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
11 Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Data Reduction by IRAF
LBC data Reduction
There is no main pipeline for reducing LBC data.
However, there are several methods to reduce LBC data.
1. LBC_redux package by Dr. Neil Crighton
https://github.com/nhmc/LBC_redux
2. LBC GUI pipeline V 1.0 (DEC2007) by INAF Astronomical
Observatory of Rome
http://lbc.oa-roma.inaf.it/commissioning/data/
LBCGUI_PIPELINE/index.html#intro
3. LBC-reduction package by Dr. Benjamin Weiner
https://github.com/bjweiner/LBC-reduction
These Methods are not easy to use. We decide to have
our own pipeline for UVa Astronomy.
https://github.com/poonpa/lbc
We use IRAF CCDRED package to reduce our data. Then
we follow our pipeline for Astrometric Calibration and
Coadding.

13. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
12 Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Astrometric Calibration and Coadding
Astrometric Calibration by SCAMP and SWARP1
By combining images using Imcombine task in IRAF, it
turn out that objects’WCS coordinates are not aligned with
Catalog’s coordinate in DS9.

14. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
13 Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Astrometric Calibration and Coadding

15. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
14 Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Astrometric Calibration and Coadding
Astrometric Calibration by SCAMP and SWARP
We decide to use SExtractor, SCAMP and SWARP2
to fix
any astrometic problem and coadding objects frames.
Here are steps
SExtractor ⇒ Retrieve catalog from all object frames
↓
SCAMP ⇒ use Retrieved catalogs and Reference catalog
to get Astrometic corrrection, stored in new header for
each object frame.
↓
SWARP ⇒ use corrected header to "Swarp" each object
frame in order to achieve correct coordinates, then stack
and combine all object frames.
↓
Now you have an astrometry corrected combined object
frames ready to be used!
2Programs by Dr. Emmanuel Bertin

16. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
15 Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Astrometric Calibration and Coadding
Figure: Zoom in of Astrometric Calibrated and Coadded Image. The
pink circles are SDSS R-6’s Catalog overlay.

17. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
16 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration
Photometric Calibration
Once we obtain an astrometric calibrated images, we have
to perform a photometric calibration.
The Photometric Calibration will allow us to understand
the Magnitude of objects i.e. derive the Magnitude
conversion equation which will convert Object’s counts in
ADU to SDSS’s r-Magnitude and g-Magnitude.

18. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
17 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration
Photometric Calibration
For objects in the SDSS database, photometric calibration
is performed in following steps
1. 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 calibration
using SExtractor’s parameters.
4. Converting SDSS’s Asinh Magnitude to Pogson Magnitude
before running the calibration.
5. Running the Calibration using IDL program.
3There are several methods to do but currently I use my own IDL program to
perform cross matching which is still not optimized.

19. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
18 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration
Photometric Calibration
Reasoning for using Pogson Magnitude instead of SDSS’s
Asinh Magnitude.
SDSS’s Asinh Magnitude was created to eliminate problem
with negative counts which is a problem in Pogson system.
Here is the SDSS Asinh Magnitude equation4
:
Mag = −(2.5/ln(10)) ∗ [asinh((f/fo)/2b) + ln(b)] (1)
fo = 10aa+kk∗Airmass5
(2)
Problem arise with Softening Parameter "b" and fo i.e.
What’s fo for our data?
Plot between SDSS’Asinh versus SExtractor’s PSF
magnitude show some non linearity.
4Lupton et al. 1999
5aa=Zero point, kk=Extinction Coefficient from Bouguer’s Law

20. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
19 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration

21. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
20 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration

22. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
21 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration

23. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
22 Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
WISE project at UVa
Photometric Calibration

24. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
23 Plan for Winter 2015 and
Spring 2016
Q&A
Question?
Contact Information
Future Plan
What’s Next?
Here are tentative goals for the Winter break and next
semester.
1. Finish Photometric Calibration for Objects in Non-SDSS
fields i.e. using different Catalog to perform calibration.
2. Finish Writing a manual for LBC data reduction,
Astrometric calibration and photometric calibration6
. This
guide will serve as a comprehensive manual for anyone at
the Astronomy Department to be able to reduce data from
the LBT archive.
3. Further study the physical properties of WISE objects as
the current reduced data allow.
6I have already create a Github page to store all required files and manual.

25. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
24 Question?
Contact Information
Q&A
Questions Time
If you have any question, please feel free to ask me.
Credit to sharelatex website. 7
7This presentation is created by LATEX

26. 25
ASTRO9995 Research
Presentation
Poon Panichpibool
AGN Project Overview
Background of the Project
Background of the Project
Research Groups
Optical Part of Project
UVa OHSU WISE project
LBT Observation
WISE project at UVa
Research Group at UVa
Current Goals
Data Reduction by IRAF
Astrometric Calibration and
Coadding
Photometric Calibration
Future Plan
Plan for Winter 2015 and
Spring 2016
Q&A
Question?
25 Contact Information
Q&A
Contact Information
In case you have any comments, suggestions or have found
additional information, please do not hesitate to contact me.
You can find my contact details below.
Poon Panichpibool
pp9mx@virginia.edu
2021 Ivy Road, Apt. B4
Charlottesville, VA 22903

27. Thank you for your attention!