C H A N D R A   S C I E N C E   C E N T E R
O B S E R V A T I O N   C A T A L O G

OBSID:
25310
 Title:
Constraining Origin of Unresolved X-ray Emission of Radio-Loud Quasars with Microlensing
Investigator:
Dai
 Observer:
Dai, Xinyu
 Phone:
6143014109
 Email:
xdai@ou.edu
Target Name:
PKS1830-211
 Sequence Number:
704354
 Instrument:
ACIS-S
 Grating:
NONE
 SI Mode:
TE_00CDCB
 Raster Scan:
N
 Annotated DOT:
OCT2722a

Proposal Number:
23700187
 Right Ascension:
278.416
 Declination:
-21.0611
 Status:
archived
 Start Date:
2022-10-27 17:22:20
Category:
ACTIVE GALAXIES AND QUASARS
 Type:
GO
 AO Cycle:
23
 Dither Flag:
Y
 Y Offset:
0
 Z Offset:
0
Est. Count Rate:
0.23
 Order-1 Count Rate:

 Exposure Time:
3
 Time Remaining:
3.104
 Reqd Start Time:

 Reqd Stop Time:
Period:

 Epoch:

 Start of Period:

 End of Period:

 PS Margin:

 PE Margin:

 Max Segments:
0

ACIS Mode:
TE
 Standard?:
No
 BEP Mode:
VF
On-Chip Summing?:
No
 Row Sum:

 Column Sum:

 Frame Time:
Subarray Mode:
CUSTOM
 Starting Row:
385
 Row Count:
256
 Subarray Frame Time:

Duty Cycle?:
No
 Cycle Count:
0
 Primary Exp Time:

 Secondary Exp Time:
Event Filter?:
No
 Filter Threshold:

 Filter Range:

 Bias Requested?:
No
 Bias Frequency:

 Bias After?:
No
 Spatial Window?:
No

Abstract:
The origin of the unresolved X-ray emission of radio-loud AGNs is still under debate, as whether it is dominated by the corona or jet emission. Emission size measurements will provide crucial constraints to distinguish the two models, since the corona emission is expected to be at least an order of magnitude smaller. While quasar microlensing analysis has been successfully applied to half a dozen of radio-quiet AGNs and yielded compact X-ray size measurements with equivalent nano-arcsec resolutions, such analysis has been performed to two radio-loud AGNs. Here, we propose to double the sample size by monitoring two radio-loud lensed quasars, such that the RL sample size is approaching the RQ size. This analysis will provide baseline emission size measurements for theoretical models.

Remarks:
The visibility window is between 2/12-10/27/2022. Ideally, the 8 monitor observations should be separated by 20-32 days. Deviations from these ideal scheduling are also acceptable, as long as they are separated by 15-37 days.

psci Run:
47
 Processing Date:
Nov 11 2022
 psci Directory:
/nfs/maaxnew/r3/fh/acis122b/acis122.log
OBSID:
25310
 SIM Mode:
ACIS-S
 OTG Mode:
NONE
 Seq Number:
704354
 Target Name:
PKS1830-211
 AO:
23
Start VCDU:
13240:112
 Start Time (UTC):
300:63496.363
 Stop Time (UTC):
300:66603.653
 Kilosecs:
3.1
 % Frames:
100.0
 # CCDs:
S2
# Frames:
3302
 # Events:
13310
 Events/sec:
4
 PSCI errors:
0
 % drops:
0.0
 Bias Errs:
0
 FP Temp:
-118.6
Parameter Block:
0x00cdc014
 Window Block:
-
 # Windows:
0
 FEP Mode:
Te5x5
 BEP Mode:
F
 Start Row:
384
 # Rows:
256
Primary Exposure:
9
 Secondary Exposure:
0
 Duty Cycle:
0
 Summing?:
No
 Bias?:
Yes
 Trickle?:
Yes
 Bias Run:
47

pgf@space.mit.edu Sat Mar 29 10:37:19 EST 2025