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OBSID:
28520
 Title:
The Lighthouse PWN as a probe of ISM structure and a unique relativistic plasma physics laboratory
Investigator:
Kargaltsev
 Observer:
Kargaltsev, Oleg
 Phone:
8144046378
 Email:
kargaltsev@gwu.edu
Target Name:
PSR J1101-6101
 Sequence Number:
503496
 Instrument:
ACIS-I
 Grating:
NONE
 SI Mode:
TE_006E6
 Raster Scan:
N
 Annotated DOT:
JUL0824a

Proposal Number:
25500121
 Right Ascension:
165.438
 Declination:
-61.0279
 Status:
observed
 Start Date:
2024-07-10 04:18:48
Category:
SN, SNR AND ISOLATED NS
 Type:
GO
 AO Cycle:
25
 Dither Flag:
Y
 Y Offset:
-0.3
 Z Offset:
0
Est. Count Rate:
0.13
 Order-1 Count Rate:

 Exposure Time:
58
 Time Remaining:
58.407
 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:
NONE
 Starting Row:
0
 Row Count:
1023
 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:
Spectacular jet-like features, extending for many parsecs from their parent pulsars and misaligned with the pulsars trajectories, have recently been unexpectedly discovered by the CXO. Being caused by rapid escape of pulsar wind e+/e- from the bow-shock head into the ISM, they illuminate the structure of the ISM magnetic field via synchrotron emission and seed the Galaxy with multi-TeV particles. The Lighthouse Nebula, with its high luminosity, filamentary structures near the pulsar, counter outflow, and large-scale bending provides an excellent laboratory to probe this phenomenon as well as properties of the ambient ISM. High resolution CXO images, with sufficient S/N to probe the fine structure, variability, and spectral trends, are the key to such study.

Remarks:
Although we requested to divide the total observing time of 700 ks equally between three CXO cycles, the actual observing times per cycle can be redistributed if it helps scheduling. Also, we do not impose any constraints on how the time is distributed within a given CXO cycle. As we do not actually request window constraints, we suppose that the correct RC is lower than calculated by CPS.

psci Run:
493
 Processing Date:
Jul 20 2024
 psci Directory:
/nfs/maaxnew/r3/fm/acis127e/acis127.log
OBSID:
28520
 SIM Mode:
ACIS-I
 OTG Mode:
NONE
 Seq Number:
503496
 Target Name:
PSR_J1101-6101
 AO:
25
Start VCDU:
30204:024
 Start Time (UTC):
192:16632.463
 Stop Time (UTC):
192:75052.288
 Kilosecs:
58.4
 % Frames:
100.0
 # CCDs:
I4
# Frames:
18599
 # Events:
816837
 Events/sec:
13
 PSCI errors:
0
 % drops:
0.0
 Bias Errs:
0
 FP Temp:
-116.4
Parameter Block:
0x006e7034
 Window Block:
-
 # Windows:
0
 FEP Mode:
Te5x5
 BEP Mode:
F
 Start Row:
0
 # Rows:
1024
Primary Exposure:
31
 Secondary Exposure:
0
 Duty Cycle:
0
 Summing?:
No
 Bias?:
No
 Trickle?:
Yes
 Bias Run:
492

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