2014A&A...567A..98M


C.D.S. - SIMBAD4 rel 1.7 - 2020.07.04CEST15:21:06

2014A&A...567A..98M - Astronomy and Astrophysics, volume 567A, 98-98 (2014/7-1)

Mid-infrared interferometry with K band fringe-tracking. I. The VLTI MIDI+FSU experiment.

MUELLER A., POTT J.-U., MERAND A., ABUTER R., DELPLANCKE-STROEBELE F., HENNING Th., KOEHLER R., LEINERT Ch., MOREL S., PHAN DUC T., POZNA E., RAMIREZ A., SAHLMANN J. and SCHMID C.

Abstract (from CDS):

A turbulent atmosphere causes atmospheric piston variations leading to rapid changes in the optical path difference of an interferometer, which causes correlated flux losses. This leads to decreased sensitivity and accuracy in the correlated flux measurement. To stabilize the N band interferometric signal in MIDI (MID-infrared Interferometric instrument), we use an external fringe tracker working in K band, the so-called FSU-A (fringe sensor unit) of the PRIMA (Phase-Referenced Imaging and Micro-arcsecond Astrometry) facility at VLTI. We present measurements obtained using the newly commissioned and publicly offered MIDI+FSU-A mode. A first characterization of the fringe-tracking performance and resulting gains in the N band are presented. In addition, we demonstrate the possibility of using the FSU-A to measure visibilities in the K band. We analyzed FSU-A fringe track data of 43 individual observations covering different baselines and object K band magnitudes with respect to the fringe-tracking performance. The N band group delay and phase delay values could be predicted by computing the relative change in the differential water vapor column density from FSU-A data. Visibility measurements in the K band were carried out using a scanning mode of the FSU-A. Using the FSU-A K band group delay and phase delay measurements, we were able to predict the corresponding N band values with high accuracy with residuals of less than 1µm. This allows the coherent integration of the MIDI fringes of faint or resolved N band targets, respectively. With that method we could decrease the detection limit of correlated fluxes of MIDI down to 0.5Jy (vs. 5Jy without FSU-A) and 0.05Jy (vs. 0.2Jy without FSU-A) using the ATs and UTs, respectively. The K band visibilities could be measured with a precision down to ≃2%.

Abstract Copyright:

Journal keyword(s): instrumentation: interferometers - techniques: interferometric - methods: observational - methods: data analysis

Simbad objects: 27

goto Full paper

goto View the reference in ADS

Number of rows : 27

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2020
#notes
1 * 33 Psc RS* 00 05 20.14193 -05 42 27.4279 6.52 5.65 4.61 3.83 3.29 K0III-IV 199 0
2 V* AD Cet LP? 00 14 27.6290894 -07 46 49.898505 8.55 6.74 5.12     M3+III 74 0
3 * iot Cet * 00 19 25.6741634 -08 49 26.111055 5.94 4.77 3.55 2.70 2.11 K1+IIICN0.5 166 0
4 * nu. Psc * 01 41 25.8939097 +05 29 15.406225 7.36 5.81 4.44 3.38 2.67 K3III 222 0
5 2MASS J02194738-1025406 TT* 02 19 47.3900688084 -10 25 40.609044310   11.80 10.72     K0e 15 0
6 * 80 Cet PM* 02 36 00.0479359493 -07 49 53.749900838   7.088 5.535     M0/1III 45 0
7 M 77 GiP 02 42 40.771 -00 00 47.84 9.70 9.61 8.87 10.1 9.9 ~ 4089 2
8 V* RY Tau Or* 04 21 57.4132838427 +28 26 35.533990877 10.82 10.34 9.30 9.67 8.87 K1IV/Ve 648 1
9 HD 27639 V* 04 22 22.7296954760 +20 49 17.091142496   7.86 5.95     M0III 44 0
10 * eps Tau ** 04 28 36.9988174 +19 10 49.544603 5.42 4.54 3.53     G9.5IIICN0.5 543 1
11 * 31 Ori V* 05 29 43.9814689897 -01 05 32.058230061   6.28 4.71     K4III 85 0
12 * del Ori A ** 05 32 00.398 -00 17 56.69           O9.5II+B1V+B0IV 25 0
13 * bet Pic PM* 05 47 17.0876901 -51 03 59.441135 4.13 4.03 3.86 3.74 3.58 A6V 1653 1
14 * tau Pup SB* 06 49 56.1684595 -50 36 52.443676   4.13 2.93     K1III 93 0
15 * tet CMa PM* 06 54 11.3997692336 -12 02 19.061054441 7.20 5.51 4.08 2.95 2.17 K3/4III 207 0
16 * 23 Car V* 07 00 51.4844144890 -51 24 09.302072576   6.770 5.151     M1III 28 0
17 V* Z CMa Ae* 07 03 43.1588002461 -11 33 06.230351311 10.51 9.99 8.80     B5/8eq+F5/7 532 3
18 HD 56470 * 07 16 16.6510592600 -21 25 14.797824905   9.98 8.45     K2/3III 5 0
19 * iot Hya PM* 09 39 51.3614457 -01 08 34.113491 6.68 5.23 3.91 2.92 2.25 K2.5III 165 0
20 * gam Cha V* 10 35 28.1071958 -78 36 28.032088 7.65 5.70 4.12 2.86 1.88 K4III 72 0
21 HD 100546 Be* 11 33 25.4404858122 -70 11 41.239343121   6.71 6.30   6.64 A0VaekB8_lB 651 1
22 V* V1068 Sco LP* 16 53 42.4238733934 -43 03 03.488567482   7.71 6.06     M3II/III 23 0
23 * zet02 Sco PM* 16 54 35.0043467 -42 21 40.740679   4.99 3.62     K3III 67 0
24 HD 155826 ** 17 15 35.9021317723 -38 35 38.168900773   6.54 5.96     G0V 78 0
25 * alf Aql dS* 19 50 46.99855 +08 52 05.9563 1.07 0.98 0.76 0.62 0.49 A7Vn 818 0
26 V* LW Aqr LP* 23 52 47.5595033267 -12 01 00.897134853   8.90 7.48     M4III 10 0
27 * 24 Psc ** 23 52 55.5634489695 -03 09 19.734659367   7.023 5.940     K0II/III 53 0

    Equat.    Gal    SGal    Ecl

To bookmark this query, right click on this link: simbad:objects in 2014A&A...567A..98M and select 'bookmark this link' or equivalent in the popup menu


2020.07.04-15:21:06

© Université de Strasbourg/CNRS

    • Contact