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This delivery contains the fifth vers= ion of the TESS Input Catalog (TIC) produced entirely by the Target Selecti= on Working Group (TSWG), and was delivered to the TESS Science Office (TSO)= on 2017 May 15.
The delivery has a number of minor is= sues (see below) which have not been fixed in this version due to time cons= traints during preparation. Specific details of the method of production an= d the contents of this TIC are described in detail in the full TIC Document= ation on the arXiv at (https://arxiv.org/abs/1706.00495) and are not repeated here.
The format used is the same as TIC-4,= in that the specific columns and their format are the same, but there have= been significant changes compared to TIC deliveries prior to TIC-5. TIC ID= s have not been changed and all future deliveries of the TIC will use the s= ame IDs for specific objects, and new objects added will receive new IDs.= span>
This delivery contains major changes = in computed quantities compared to TIC-4. It should be noted the methods us= ed to estimate a variety of the stellar parameters are still under active d= evelopment and can be affected by poor catalog photometry when there is no = acceptable alternative photometry for a given star. The major changes compa= red to previous versions are:
An internal database error in the reduced proper motion selection = in TIC-4 was corrected. Originally, this error resulted in ~11 million like= ly dwarfs being excluded from the TIC-4 CTL and ~600K stars which are likel= y giants being included in the CTL. The contaminants have been removed and = the possible dwarfs included in the new CTL selection (see 5 & 6 below)= .
We now define a 0.05 mag area to the left of V-Ks =3D 2.2241 above= the polynomial fit to the data from Bessell & Brett, 1988 (see Figure = 10 in the documentation). Stars within this area are assumed to have 0 redd= ening and have been flagged as 'dered0'.
We now select a maximum E(B-V) value of 1.5 rather than 15.=
The priority calculation has been updated to properly combine TESS= =E2=80=99s expected photometric precision and the expected contamination ra= tio for a given source. The contamination ratio and photometric error are n= ow combined as sqrt(=CE=B5+1)*(=CF=83*10^-6), where =CE=B5 is the contamina= tion ratio and =CF=83 is the expected photometric precision in ppm.<= /p>
In addition to requiring CTL stars to be RPMj dwarfs and have T &l= t; 15 (unless in a special target list), the CTL now excludes stars where T= > 12 and Teff > 5500 K.
Any star with J-H > 0.75 is now excluded from the CTL (even if = it is identified as a reduced proper motion dwarf) unless it is included in= the cool dwarf list or has a spectroscopic Teff.
We have implemented a variety of internal consistency checks to en= sure parameters such as mass, radius, log(g) etc are all internally consist= ent within the reported values for any given star in the TIC. See Appendix = D of the documentation for more details.
Stars within 15 deg of the Galactic Plane (|b| < 15) have their= priorities de-boosted by a factor of 0.1.
Minor fixes and exclusions of stars left in the CTL from legacy ve= rsions of the cool dwarf list.
The contamination ratio no longer uses galaxies as possible contam= inants. The galaxy distribution is expected to be homogenous across the sky= and eliminating the galactic contamination relieves much of the structure = present in the distribution of top priority CTL targets.
The CTL now incorporates a =E2=80=9CBright Star=E2=80=9D specially= curated target list. This includes all stars in the TIC with T<6. Conta= mination ratios were calculated for this target list and priority values we= re set to be 1. These stars, in most cases, do not have all stellar paramet= ers, such as mass and radii, calculated.
No. Name Notes
2 Version &= nbsp; This co= lumn denotes the date YYYYMMDD, in which the TIC was delivered to the POC. = A typo left the date as 20160515, it should be 20170515.
7 SDSS The values given are the 64-bit "obj= ID" values, not the IAU-format "SDSSJ" identifiers.
9
10 APASS APASS stars do not have an identifier=
, only coordinates. We use the primary key of an internal TESS version of the APASS database table as a=
proxy identifier.
17
19
22 29 59 61 Tmag &nbs=
p;This column is never NULL. The =
Tmag values are typically based on relations that depend on J and V-Ks or J-Ks (see column 63 for metho=
d flag). TESS magnitudes for objects for which only poor catalog photometry=
was available were computed simply as offsets from a reference magnitude (=
see Documentation Section 2.2.2). 63 TESSflag See TIC-5 Documentation Section 2.2.1 for detail=
s of each method. While most of these relations (which are used for most Tm=
ag values) are only appropriate for dwarf stars, some are applicable to gia=
nts. Extended objects were treated as if they were dwarfs. In general the d=
warf relations are strictly valid between specific color ranges and tend to=
be less accurate for very blue stars (J-Ks < -0.1) or very red stars (J=
-Ks > 1). These flags den=
ote which relation or catalog provides the TIC TESS magnitude: &n=
bsp; hipvmag:=
T calculated from Cool Dwarf list (see Documentation Section E.1.1 and Muirhead et al. (2017 in prep)<=
/span> &n=
bsp; cdwarf: =
T calculated from Cool Dwarf list (see Documentation Section &n=
bsp; from_apa=
ss_i: T calculated from cdwarf catalog (see Sec. E.1.1 & Muirhead=
et al. 2017) &n=
bsp; from_sds=
s_i: T calculated from cdwarf catalog (see Sec. E.1.1 & Muirhead =
et al. 2017) &n=
bsp; wmean_vk=
_jhk: T calculated from cdwarf catalog (see Sec. E.1.1 & Muirhead=
et al. 2017) E.1.1 and Muirhead et al. (2017 in prep)=
span>
= &nb= sp; joffset: Tmag calculate= d from 2MASS J + offset.
= &nb= sp; koffset: Tmag calculate= d from 2MASS Ks + offset.
= &nb= sp; lepine: Tmag calculated= using the V magnitude from the Lepine catalog
= &nb= sp; bpjk: Relation using 2M= ASS JKs and photographic B.
= &nb= sp; jhk: Relation using 2MA= SS JHKs.
= &nb= sp; vjk: Relation using 2MA= SS JKs and Johnson V.
= &nb= sp; voffset: Tmag calculate= d from V + offset.
= &nb= sp; tmvk: Relation using 2M= ASS calculated V and Ks.
= &nb= sp; jh: Relation using 2MAS= S JH.
= &nb= sp; sdss: Relation for exte= nded objects using Sloan g and i.= 64= SPFlag These flags denote the origin of stell= ar characteristics:
&n= bsp; <= span style=3D"color: rgb(0,0,0);">cdwarf: mass and radius provided by the C= ool Dwarf list
= &n= bsp; plx: characteris= tics computed from measured parallax
= &n= bsp; spect:characte= ristics computed using the spectroscopic Torres relations
=
<=
/span> &=
nbsp; allen: charact=
eristics computed from spline relations based on eclipsing
= &n= bsp; normal: same as = allen, naming artifact to be removed in future releases
65= Teff = ; The effective temperatures come from one of four so= urces, in the following orde= r of preference: (1) the Cool Dwarf list; (2) spectroscopic catalogs (see C= olumn 64); (3) dereddended V-Ks color; and (4) non-dereddened V-Ks color. &= nbsp;Please note that all stars with Teff < 3840 K have been excluded fr= om any de-reddening, on the assumption that they are nearby M dwarfs.
66= e_Teff<= /span>&nb= sp; The SPOCS and GALAH catalogs do not provide uncertainties for&n= bsp;effective temperatures; 25K a= nd 41K were assigned, respectively, based on the reported statistical error= from those catalogs.
67=
Logg
68=
e_Logg<=
/span>&nb=
sp; T=
he SPOCS and GALAH catalogs do not provide uncertainties for surface gravities; 0.028 and 0.17 dex were=
assigned, respectively, based on the reported statistical error from those=
catalogs.
70= e_M/H= span>&nbs= p; The SPOCS and GALAH catalogs do not provide uncertainties for metallicities; 0.10 and 0.05 dex were= assigned, respectively, based on the reported statistical error from that = catalog.
71= Mass = ; If an object=E2=80=99s mass is provided in the specialized Cool D= warf list it is included in = the TIC. Otherwise, the stellar masses were estimated using a relation base= d on measured masses for eclipsing binaries as well as simulations using Ga= lactic structure models.
73= Radius<= /span>&nb= sp; The stellar radii were estimated using a variety of techniques, in the&= nbsp;following order of preferenc= e: (1) the Cool Dwarf list; (2) spectroscopic relations from Torres et al. = 2010, A&ARv, 18, 67; (3) using the Gaia parallax and bolometric correct= ions; and (4) a unified relation based on measured radii for eclipsing bina= ries as well as simulations using Galactic structure models.
77= LumClas= s This is a boolean d= warf flag. If this is set, LumClass =3D DWARF, or otherwise GIANT. SUBGIANT is not used at pres= ent. However, the DWARF flag for TIC-5 effectively means that the star is e= ither a dwarf or a subgiant, based on reduced proper motion cuts.
82= E(B-V)<= /span>&nb= sp; Stars for which E(B-V) > 1.5 have their E(B-V) values set to a maxim= um of 1.5.
85= contrat= io= The co= ntamination ratio is defined as the nominal flux from the contaminants divided by the flux from the sou= rce. Flux contamination is calculated for all stars identified as dwarfs th= at are brighter than Tmag=3D15, or are in special target catalogs such as t= he Cool Dwarf list. Contaminants are searched for within 10 TESS pixels of = the target and the contaminating flux is calculated within a radius that de= pends on the target=E2=80=99s Tmag. The PSF is modeled using a 2D-Gaussian = based on preliminary PSF measurements from the SPOC.
88= priorit= y Priority of target for observation. This is a floating-point value ranging= from 0 to 1, where 1 is hig= hest priority. The priority is based on the relative ability of TESS to det= ect small planetary transits, and is calculated using the radius of the sta= r, the contamination ratio, and the total expected photometric precision. S= tars within the continuous viewing zones (|b| > ~78 deg) are given a boo= st to their priority by a factor of sqrt(13), as they will be observed roug= hly 13 times longer than the majority of TESS targets. Stars within the Gal= actic Plane (|b|<15) have been de-boosted by a factor of 0.1 since we ge= nerally have a poor understanding of their true de-reddening.
No. Name
83 e_EBV
86 Disposition
There are a number of minor issues wh= ich have been identified by the TSWG. We expect to address these issues in = a future version of the TIC. The issues include:
All coordinates are for the epoch of observation (often 2MASS or S= DSS). Epochs are not currently supplied.
Because some stars have poor quality 2MASS photometry flags (such = as =E2=80=98D=E2=80=99, =E2=80=98U=E2=80=99), offsets where applied to V, J= , H, or Ks magnitudes to provide a more realistic TESS magnitude but may be= different from the true value by a magnitude or more.
There is a clear pattern in the sky distribution of top CTL stars.= This is a combination of three effects: The first is from the SuperB= link/UCAC4/Proper Motion Catalogs. The edge at ~-30 deg is due to the incom= pleteness in these catalogs. The second effect is the priority boost to sta= rs in the CVZ, typically any star with an ecliptic latitude greater than 78= is more likely to have a high priority. The third effect is the priority d= e-boost to stars within 15 degrees of the Galactic Plane by a factor of 0.1= .
A typo left the Version date as 20160= 515, it should be 20170515.
The surface gravities reported in column 67 of TIC-5,do not accura= tely represent the expected surface gravities using the reported values for= mass (column 73) and radii (column 71). This only affects stars where the = stellar properties were calculated using available parallax information (th= e stellar properties flag is set to 'plx' in column 64) and no other quanti= ties in the TIC are affected. TIC users can either calculate the surface gr= avity using the provided mass and radius values or use the linked data file= (http://astro.phy.vanderbilt.edu= /~oelkerrj/ftp/tic5_logg_fix.csv) to access the appropriately calculate= d values. This fix will be built into the next version of the TIC, version = 6.
For TIC-5, numerical columns with values of exactly 0 are actually= null values. Starting in TIC-6, these will be properly set to null, but du= e to a translation error they have been assigned values of exactly 0 in TIC= -5 at MAST.
There are a number of planned improve= ments for the future versions of the TIC. At present these improvements inc= lude:
A refinement of the algorithm for calculating the expected photome= tric error based on Tmag to include properties such as the coordinates, to = properly account for zodiacal light.
All coordinates to be prepared in equinox J2000.0, and epoch 2000.= 0.
Create a more extensive list of stars with known radii and masses,= so that we can test expanded mass and radius relations.
Fully incorporate Gaia magnitudes into the calculation of Tmag, po= sitions, and source IDs.
Improve dwarf/sub-giant/giant classification using Gaia parallax i= nformation.