2023PASP..135a5003S

Query : 2023PASP..135a5003S

2023PASP..135a5003S - Publ. Astron. Soc. Pac., 135, part no 1, 5003 (2023/January-0)

The Near Infrared Imager and Slitless Spectrograph for the James Webb Space Telescope. IV. Aperture Masking Interferometry.

SIVARAMAKRISHNAN A., TUTHILL P., LLOYD J.P., GREENBAUM A.Z., THATTE D., COOPER R.A., VANDAL T., KAMMERER J., SANCHEZ-BERMUDEZ J., POPE B.J.S., BLAKELY D., ALBERT L., COOK N.J., JOHNSTONE D., MARTEL A.R., VOLK K., SOULAIN A., ARTIGAU E., LAFRENIERE D., WILLOTT C.J., PARMENTIER S., FORD K.E.S., McKERNAN B., VILA M.B., ROWLANDS N., DOYON R., BEAULIEU M., DESDOIGTS L., FULLERTON A.W., DE FURIO M., GOUDFROOIJ P., HOLFELTZ S.T., LAMASSA S., MASZKIEWICZ M., MEYER M.R., PERRIN M.D., PUEYO L., SAHLMANN J., SOHN S.T., TEIXEIRA P.S. and ZHENG S.-H.

Abstract (from CDS):

The James Webb Space Telescope's Near Infrared Imager and Slitless Spectrograph (JWST-NIRISS) flies a 7-hole non-redundant mask (NRM), the first such interferometer in space, operating at 3-5 μm wavelengths, and a bright limit of ≃4 mag in W2. We describe the NIRISS Aperture Masking Interferometry (AMI) mode to help potential observers understand its underlying principles, present some sample science cases, explain its operational observing strategies, indicate how AMI proposals can be developed with data simulations, and how AMI data can be analyzed. We also present key results from commissioning AMI. Since the allied Kernel Phase Imaging (KPI) technique benefits from AMI operational strategies, we also cover NIRISS KPI methods and analysis techniques, including a new user-friendly KPI pipeline. The NIRISS KPI bright limit is ≃8 W2 (4.6 μm) magnitudes. AMI NRM and KPI achieve an inner working angle of ∼70 mas, which is well inside the ∼400 mas NIRCam inner working angle for its circular occulter coronagraphs at comparable wavelengths.

Abstract Copyright: © 2023. The Astronomical Society of the Pacific. All rights reserved.

Journal keyword(s): High angular resolution - Interferometers - Direct detection interferometry - Astronomy data reduction

Simbad objects: 17

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Number of rows : 17
N Identifier Otype ICRS (J2000)
RA 		ICRS (J2000)
DEC 		Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2024 		#notes
1 M 77 Sy2 02 42 40.7091669408 -00 00 47.859690204 9.70 9.61 8.87 10.1 9.9 ~ 4607 2
2 EM* LkCa 15 Or* 04 39 17.7911622816 +22 21 03.390090984   13.01 12.03 11.61   K5:Ve 690 1
3 V* AB Dor C LM* 05 28 44.83 -65 26 54.9           M8: 67 0
4 V* AB Dor TT* 05 28 44.8712165880 -65 26 55.199147208 8.259 7.856 6.999 6.496 5.993 K0V 1023 0
5 HD 36805 * 05 29 06.4770554328 -66 41 13.201208412   9.36 8.09     K2III 23 0
6 HD 37093 * 05 31 08.2590174816 -65 07 42.083399712   10.70 9.25     K5(III) 13 0
7 TYC 8906-1660-1 * 06 27 00.5443408200 -66 21 59.052159720   12.24 10.64     ~ 3 0
8 UCAC4 117-011267 * 06 28 02.0014566936 -66 37 38.095571100   11.979   10.708   ~ 4 0
9 CPD-67 607 * 06 29 31.9252018176 -67 13 13.004316048   11.784 10.732     ~ 6 0
10 CPD-66 562 * 06 31 36.6171205438 -66 21 47.605754007   11.344 10.511     ~ 8 0
11 HD 95086 * 10 57 03.0215719872 -68 40 02.449216128   7.60 7.36     A8III 177 1
12 HD 100546 Be* 11 33 25.4408872296 -70 11 41.241297948   6.71 6.30   6.64 A0VaekB8_lB 806 1
13 * eta Crv PM* 12 32 04.2264018482 -16 11 45.618615379   4.658 4.294     F2V 318 0
14 HD 115600 * 13 19 19.5409822176 -59 28 20.441034660   8.59 8.22     F2IV/V 71 1
15 CD-40 8434 TT* 14 08 10.1545500744 -41 23 52.573291080   13.42 12.18 11.71 10.506 K7IVe 360 0
16 CPD-36 6759 Y*O 15 15 48.4460065200 -37 09 16.024369824   9.21 8.708     F8V 463 1
17 HD 218396 El* 23 07 28.7157209544 +21 08 03.310767492   6.21 5.953     F0+VkA5mA5 1139 0

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