HD 13755   A late-type {lambda} Boo star showing a small excess in the W4 band. Photometry in that band is given an "A" quality by the AllWISE Source Catalog;
HD 68695   An emission-line Ae star with large IR excesses even in the 2MASS J, H, and K bands (see Table 4). Folsom et al. (2012MNRAS.422.2072F) carried out an abundance analysis for this star, and found "clear {lambda} Boo peculiarities" with C, N, O, and S abundances that are 1{sigma} above solar and iron peak abundances 2-3{sigma} below solar. Our visual classification of this star concurs with their conclusion that this is an Ae {lambda} Boo star with strong emission at H{beta}. Murphy et al. 2015 (Cat. J/other/PASA/32.36) however, obtained two classification spectra of this star, and found it to be a spectrum variable and concluded that it did not appear to be a {lambda} Boo star. Their spectral type (A3 Ve kA1mA0) is almost identical to ours, however;
HD 81290   F4 V kA3mA3 {lambda} Boo? If this star proves to be a {lambda} Boo star, it will be the latest spectral-type {lambda} Boo star known. K.-P. Cheng (2017, private communication) has noted that HD 81290 has a CI/MgII ratio (cf. Cheng et al. 2017AJ....153...39C) that is consistent with a {lambda} Boo designation. Table 4 records an excess in the WISE W4 band. However, according to the AllWISE Source Catalog, that excess may be due to a latent image left from a bright source;
HD 100546  Acke & Waelkens (2004A&A...427.1009A) found, from an abundance analysis that this Herbig Ae star has solar nitrogen and oxygen abundances, but ~1 dex under-abundances of magnesium, silicon, and iron. Our spectrum shows strong emission in the core of H{beta}, and asymmetric infilling of all the higher Balmer lines. The Balmer line wings are consistent with an A0 Va spectral type (although B9.5 Vb is also possible), a helium line spectral type of B9.5, but a B8 metallic-line type (judged from the Ca II K-line and the Mg II 4481{AA} line). Thus, we concur with the metal-weak nature of this star, and agree with the {lambda} Boo designation. See Pascual et al. (2016A&A...586A...6P) for a plot of its stellar energy distribution (SED);
HD 101412  Folsom et al. (2012MNRAS.422.2072F) concluded from an abundance analysis that this Ae star has solar abundances of C, O, and He, with under-abundances in the iron peak elements, characteristic of a {lambda} Boo star. Their analysis agreed closely with that of Cowley et al. (2010A&A...523A..65C), who also noted that its abundance pattern was similar to that of a {lambda} Boo star. Interestingly, this star is magnetic with a longitudinal field of 500+/-100G (Folsom et al. 2012MNRAS.422.2072F). Our spectral type supports its status as a {lambda} Boo star, in agreement with Murphy et al. 2015 (Cat. J/other/PASA/32.36). Our IR analysis finds strong excesses even in the 2MASS J, H, and K bands;
HD 139614  An abundance analysis by Folsom et al. (2012MNRAS.422.2072F) found "a clear {lambda} Boo pattern of abundances with solar C, N, and O, and under-abundant iron peak elements in this Ae star. Acke & Waelkens (2004A&A...427.1009A), however, while agreeing with an overall metal-weak nature, did not find evidence for solar abundances for C, N, and O. Folsom et al. (2012MNRAS.422.2072F) attributed that disagreement to the higher T_eff_ assigned by Acke & Waelkens (8000K to their 7600K). Our T_eff_ is in better agreement with Folsom et al. (2012MNRAS.422.2072F) (7500K), and our spectral type does indeed suggest this is a mild {lambda} Boo star. Murphy et al. 2015 (Cat. J/other/PASA/32.36) likewise conclude that it is a {lambda} Boo star. Our IR analysis shows strong IR excesses even at 2MASS J, H, and K;
HD 141569  Folsom et al. (2012MNRAS.422.2072F) find a {lambda} Boo abundance pattern in this Ae star consistent with a mild {lambda} Boo character. Gray & Corbally (1998AJ....116.2530G) classified this star as metal-weak, but did not assign a {lambda} Boo type. Our spectral type A2 Ve kB9mB9 ({lambda} Boo) is significantly different from that of Gray & Corbally (1998AJ....116.2530G)--kB9 A0Va-(e)--suggesting a spectrum variable. See Pascual et al. (2016A&A...586A...6P) for a plot of its SED;
HD 142994  A late-type {lambda} Boo star showing significant excesses in the W2, W3, and W4 bands. The photometry in those bands is listed as "A" quality in the AllWISE Souce Catalog;
HD 154153  First classified as a {lambda} Boo star by Paunzen (2001A&A...373..633P), this star has a late spectral type (F1) for a {lambda} Boo star, but shows sizeable infrared excesses in the WISE W1 (3.35{mu}m) and W2 (4.6{mu}m) bands, and smaller excesses at W3 and W4. However, according to the AllWISE point-source catalog, that photometry may be contaminated by a halo from a nearby bright star. Spitzer IRAC 3.6 and 4.5{mu}m photometry, on the other hand, are consistent with no infrared excesses in that wavelength range;
HD 169142  Folsom et al. (2012MNRAS.422.2072F) detected a "clear {lambda} Boo pattern of abundances". Our spectrum shows clear infilling of the H{beta} line as well as H{gamma}, as well as a clearly metal-weak character. The literature is unclear about the {lambda} Bootis nature of this star (see Murphy et al. 2015, Cat. J/other/PASA/32.36), but our spectrum shows clear {lambda} Boo characteristics. It appears to be a spectrum variable, and it would be of interest to follow this star for a period of time to see if its {lambda} Bootis nature also varies. See Pascual et al. (2016A&A...586A...6P) for a plot of its SED;
HD 183007  We concur with Murphy et al. 2015 (Cat. J/other/PASA/32.36) that this star has a composite spectrum, but differ from them in not assigning a {lambda} Boo type, largely because of the inconsistency between the K-line and the metallic-line types;
HD 188164  Classified by Paunzen et al. (1996IBVS.4302....1P) as {lambda} Boo(?), but by Paunzen et al. 2001 (Cat. J/A+A/373/625) as A3 V (e.g., normal), this star does appear from our spectra to be mildly metal-weak (A6 V kA2mA3). Murphy et al. 2015 (Cat. J/other/PASA/32.36) consider it an extremely mild, but bona fide {lambda} Boo star, although with the caveat that a full abundance analysis is necessary for certainty. We prefer to err on the cautious side, and call this star a possible, although very mild, {lambda} Boo star. It is a spectroscopic binary and does show a slight excess in the WISE W2 band, although not at W3 or W4;
HD 217813  An A2 V shell star that shows IR excesses consistent with the presence of a cooler companion. Those IR excesses can be accounted for within the errors by a 4900K companion with a bolometric luminosity 0.6 times that of the visible component. No parallax is available for HD 217813. Adopting M_V_=1.9 for the visible component (Gray & Corbally 2009ssc..book.....G) and applying appropriate bolometric corrections from Flower 1996 (Cat. J/ApJ/469/355), this yields, for the companion, L=8.7L_{Sun}_, which would place the companion star at the base of the red-giant branch. The shell features in the spectrum may arise from mass transfer in this possible Algol system;
BD-13 6465 This star has been variously classified in the literature as a high-latitude spectroscopically peculiar star (A2pec, Graham & Slettebak 1973AJ.....78..295G), a subdwarf sdB5 (deduced from Vilnius photometry, Bartkevicius & Lazauskaite 1997BaltA...6..499B), and a young runaway star (Tetzlaff et al. 2011, Cat. J/MNRAS/410/190). Our spectral type, F1 V kA2mA3, suggests either a late-type {lambda} Boo star or an F1 intermediate population II star. Its high galactic latitude (-69{deg}) yields a very low reddening along its line of sight (~0.02mag, Schlafly & Finkbeiner 2011ApJ...737..103S). Assuming zero reddening, the Gaia parallax (3.01+/-0.30mas, Gaia Collaboration et al. 2016A&A...595A...2G; 2016, Cat. I/337) implies an absolute magnitude M_V_=2.97+/-0.21. This, combined with B-V=0.29, is consistent with an F-type dwarf. Its space velocity components relative to the local standard of rest are U=-43km/s, V=2km/s, and W=0km/s, consistent with the young thin-disk population. An abundance analysis will be required to decide on the nature of this interesting star;
CD-31 306  This star has been classified in the literature as a blue straggler star (cf. Carney et al. 2005AJ....129..466C), a candidate HB star (Beers et al. 2007, Cat. J/ApJS/168/277), and a carbon-enhanced metal-poor star (Preston & Sneden 2000AJ....120.1014P). Our classification is F3 V kA2mA2 V, but the spectrum, which is clearly metal-weak, is sufficiently noisy that we cannot distinguish among those possibilities.